Sample records for binary floating-point number

  1. A floating-point processor for the Texas Instruments model 980A computer

    E-Print Network [OSTI]

    Brinkmann, Hubert Eldie

    1977-01-01T23:59:59.000Z

    OF SCIENCE May 1977 Major Subject: Flectrical Engineering A FLOATING-POINT PROCESSOR FOR THE TEXAS INSTRUMENTS MODEL 980A COMPUTER A Thesis by HUBERT ELDIE BRINKMANN, JR. Approved as to style and content by: C airman o. Committee) Hea , Depar ent... part of the subtrahend has been two's complemented. Floating-Point Multiplication After the characteristic and mantissa have been separated, t?o characteristics of the two numbers are added and the mantissas are multiplied to initiate...

  2. Accelerating Pipelined Integer and Floating-Point Accumulations in Configurable

    E-Print Network [OSTI]

    Martonosi, Margaret

    Accelerating Pipelined Integer and Floating-Point Accumulations in Configurable Hardware addition until the end of a repeated calculation such as accumulation or dot- product; this effectively and floating- point designs that use our technique. Our pipelined integer multiply-accumulate (MAC) design

  3. Evaluating Energy Efficiency of Floating Point Matrix Multiplication on FPGAs

    E-Print Network [OSTI]

    Prasanna, Viktor K.

    Evaluating Energy Efficiency of Floating Point Matrix Multiplication on FPGAs Kiran Kumar Matam, prasanna}@usc.edu Abstract--Energy efficiency has emerged as one of the key performance metrics in scientific computing. In this work, we evaluate the energy efficiency of floating point matrix multipli

  4. A bit-serial floating point multiply/add architecture for signal processing applications

    E-Print Network [OSTI]

    Williams, Bertrand Jeffery

    1983-01-01T23:59:59.000Z

    the order and size of the sign, exponent, and mantissa of t' he floating point number. The value of the radix ls also specified by the format. For a bit-serial floating point architecture consideration must be given to the order In e (i) b3 0 D a2 b2... silicon chip. Design complexity fs evaluated by the area requirements of the circuitry at the technology resolution of a 0. 2 mi I (5 um) minimum gate size. This would allow perhaps 10, 000 transistors on a 200 ml1 square of silicon (15, 16, 17, 18...

  5. Built-in Treatment of an Axiomatic Floating-Point Theory for SMT Solvers

    E-Print Network [OSTI]

    Andrews, Peter B.

    Built-in Treatment of an Axiomatic Floating-Point Theory for SMT Solvers Sylvain Conchon LRI-point numbers is out of reach of current SMT solvers, especially when it comes to automatic reasoning an interface akin to the instantiation mechanism of an SMT solver. This procedure is based on the approach

  6. Roofline: An Insightful Visual Performance Model for Floating-Point Programs and Multicore Architectures

    SciTech Connect (OSTI)

    Williams, Samuel; Waterman, Andrew; Patterson, David

    2009-02-01T23:59:59.000Z

    We propose an easy-to-understand, visual performance model that offers insights to programmers and architects on improving parallel software and hardware for floating point computations.

  7. Floating point only SIMD instruction set architecture including compare, select, Boolean, and alignment operations

    DOE Patents [OSTI]

    Gschwind, Michael K. (Chappaqua, NY)

    2011-03-01T23:59:59.000Z

    Mechanisms for implementing a floating point only single instruction multiple data instruction set architecture are provided. A processor is provided that comprises an issue unit, an execution unit coupled to the issue unit, and a vector register file coupled to the execution unit. The execution unit has logic that implements a floating point (FP) only single instruction multiple data (SIMD) instruction set architecture (ISA). The floating point vector registers of the vector register file store both scalar and floating point values as vectors having a plurality of vector elements. The processor may be part of a data processing system.

  8. A Floating-point Accumulator for FPGA-based High Performance Computing Applications

    E-Print Network [OSTI]

    Zambreno, Joseph A.

    A Floating-point Accumulator for FPGA-based High Performance Computing Applications Song Sun Joseph,zambreno}@iastate.edu Abstract--A floating-point accumulator for FPGA-based high performance computing applications is proposed and evaluated. Compared to previous work, our accumulator uses a fixed size circuit, and can reduce an arbitrary

  9. FLOATING-POINT BIT-WIDTH OPTIMIZATION FOR LOW-POWER SIGNAL PROCESSING APPLICATIONS

    E-Print Network [OSTI]

    Chen, Tsuhan

    FLOATING-POINT BIT-WIDTH OPTIMIZATION FOR LOW-POWER SIGNAL PROCESSING APPLICATIONS Fang Fang design flow to the design of inverse discrete cosine transform (IDCT), and show that the power floating-point (FP) signal processing applications in low-power mobile devices, we propose a lightweight FP

  10. High-Precision Floating-Point Arithmetic in ScientificComputation

    SciTech Connect (OSTI)

    Bailey, David H.

    2004-12-31T23:59:59.000Z

    At the present time, IEEE 64-bit floating-point arithmetic is sufficiently accurate for most scientific applications. However, for a rapidly growing body of important scientific computing applications, a higher level of numeric precision is required: some of these applications require roughly twice this level; others require four times; while still others require hundreds or more digits to obtain numerically meaningful results. Such calculations have been facilitated by new high-precision software packages that include high-level language translation modules to minimize the conversion effort. These activities have yielded a number of interesting new scientific results in fields as diverse as quantum theory, climate modeling and experimental mathematics, a few of which are described in this article. Such developments suggest that in the future, the numeric precision used for a scientific computation may be as important to the program design as are the algorithms and data structures.

  11. Verification of Floating-Point Adders Yirng-An Chen and Randal E. Bryant

    E-Print Network [OSTI]

    Bryant, Randal E.

    Verification of Floating-Point Adders ¡ Yirng-An Chen and Randal E. Bryant yachen+@cs.cmu.edu, bryant+@cs.cmu.edu Computer Science Dept., Carnegie Mellon Univ., Pittsburgh, PA 15213 Abstract

  12. Generating and executing programs for a floating point single instruction multiple data instruction set architecture

    DOE Patents [OSTI]

    Gschwind, Michael K

    2013-04-16T23:59:59.000Z

    Mechanisms for generating and executing programs for a floating point (FP) only single instruction multiple data (SIMD) instruction set architecture (ISA) are provided. A computer program product comprising a computer recordable medium having a computer readable program recorded thereon is provided. The computer readable program, when executed on a computing device, causes the computing device to receive one or more instructions and execute the one or more instructions using logic in an execution unit of the computing device. The logic implements a floating point (FP) only single instruction multiple data (SIMD) instruction set architecture (ISA), based on data stored in a vector register file of the computing device. The vector register file is configured to store both scalar and floating point values as vectors having a plurality of vector elements.

  13. Preliminary Results of a RANS Simulation for a Floating Point Absorber Wave Energy System Under Extreme Wave Conditions

    SciTech Connect (OSTI)

    Yu, Y.; Li, Y.

    2011-10-01T23:59:59.000Z

    This paper presents the results of a preliminary study on the hydrodynamics of a moored floating-point absorber (FPA) wave energy system under extreme wave conditions.

  14. Software Aspects of IEEE Floating-Point Computations for Numerical Applications in High Energy Physics

    ScienceCinema (OSTI)

    None

    2011-10-06T23:59:59.000Z

    Floating-point computations are at the heart of much of the computing done in high energy physics. The correctness, speed and accuracy of these computations are of paramount importance. The lack of any of these characteristics can mean the difference between new, exciting physics and an embarrassing correction. This talk will examine practical aspects of IEEE 754-2008 floating-point arithmetic as encountered in HEP applications. After describing the basic features of IEEE floating-point arithmetic, the presentation will cover: common hardware implementations (SSE, x87) techniques for improving the accuracy of summation, multiplication and data interchange compiler options for gcc and icc affecting floating-point operations hazards to be avoided About the speaker Jeffrey M Arnold is a Senior Software Engineer in the Intel Compiler and Languages group at Intel Corporation. He has been part of the Digital->Compaq->Intel compiler organization for nearly 20 years; part of that time, he worked on both low- and high-level math libraries. Prior to that, he was in the VMS Engineering organization at Digital Equipment Corporation. In the late 1980s, Jeff spent 2½ years at CERN as part of the CERN/Digital Joint Project. In 2008, he returned to CERN to spent 10 weeks working with CERN/openlab. Since that time, he has returned to CERN multiple times to teach at openlab workshops and consult with various LHC experiments. Jeff received his Ph.D. in physics from Case Western Reserve University.

  15. Co-synthesis of FPGA-Based Application-Specific Floating Point SIMD Accelerators

    E-Print Network [OSTI]

    Wong, Weng Fai

    ,wongwf}@comp.nus.edu.sg ABSTRACT The constant push for feature richness in mobile and em- bedded devices has significantly-design toolchain that generates code and application-specific platform extensions that implement SIMD instructions-tuning the application, including conversion to fixed point and then tackling the precision issue. Yet, floating point

  16. Experiments on the feasibility of using a floating-point simplex in an SMT solver

    E-Print Network [OSTI]

    Monniaux, David

    Experiments on the feasibility of using a floating-point simplex in an SMT solver Diego C B de, France david.monniaux@imag.fr Abstract SMT solvers use simplex-based decision procedures to solve. State- of-art SMT solvers use rational (exact) simplex implementations, which have shown good

  17. A Software-Oriented Floating-Point Format for Enhancing Automotive Control Systems

    E-Print Network [OSTI]

    Hwu, Wen-mei W.

    A Software-Oriented Floating-Point Format for Enhancing Automotive Control Systems Daniel A, yamada, hwug@crhc.uiuc.edu August 11, 1999 In recent years, the software of automotive control sys- tems- ber computation in automotive control systems by design- ing a new software-oriented floating

  18. An analysis of the double-precision floating-point FFT on FPGAs.

    SciTech Connect (OSTI)

    Hemmert, K. Scott; Underwood, Keith Douglas

    2005-01-01T23:59:59.000Z

    Advances in FPGA technology have led to dramatic improvements in double precision floating-point performance. Modern FPGAs boast several GigaFLOPs of raw computing power. Unfortunately, this computing power is distributed across 30 floating-point units with over 10 cycles of latency each. The user must find two orders of magnitude more parallelism than is typically exploited in a single microprocessor; thus, it is not clear that the computational power of FPGAs can be exploited across a wide range of algorithms. This paper explores three implementation alternatives for the fast Fourier transform (FFT) on FPGAs. The algorithms are compared in terms of sustained performance and memory requirements for various FFT sizes and FPGA sizes. The results indicate that FPGAs are competitive with microprocessors in terms of performance and that the 'correct' FFT implementation varies based on the size of the transform and the size of the FPGA.

  19. Logic Design Chapter 1: Binary Numbers

    E-Print Network [OSTI]

    Wu, Xiaolin

    of four bits: nibble · A group of eight bits: byte Conversion between Decimal and Binary · Converting least-significant bit (LSB) · The left most bit is called the most significant bit (MSB) · A group

  20. Experimental Investigation of the Power Generation Performance of Floating-Point Absorber Wave Energy Systems: Preprint

    SciTech Connect (OSTI)

    Li, Y.; Yu, Y.; Epler, J.; Previsic, M.

    2012-04-01T23:59:59.000Z

    The extraction of energy from ocean waves has gained interest in recent years. The floating-point absorber (FPA) is one of the most promising devices among a wide variety of wave energy conversion technologies. Early theoretical studies mainly focused on understanding the hydrodynamics of the system and on predicting the maximum power that could be extracted by a heaving body. These studies evolve from the investigation of floating-body interactions in offshore engineering and naval architecture disciplines. To our best knowledge, no systematic study has been reported about the investigation of the power generation performance of an FPA with a close-to-commercial design. A series of experimental tests was conducted to investigate the power extraction performance of an FPA system.

  1. Supporting De-normalized Numbers in an IEEE Compliant Floating-Point

    E-Print Network [OSTI]

    Beimel, Amos

    Yariv Levin Tel-Aviv University Electrical Engineering Department 69978 Tel-Aviv Israel July 2001 Environment 60 9 Summary and Discussion 62 A Additional Required Designs 64 A.1 Recoding Modules . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 64 A.2 Priority Encoding . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 64 A.3

  2. RANS Simulation of the Heave Response of a Two-Body Floating Point Wave Absorber: Preprint

    SciTech Connect (OSTI)

    Yu, Y.; Li, Y.

    2011-03-01T23:59:59.000Z

    A preliminary study on a two-body floating wave absorbers is presented in this paper. A Reynolds-Averaged Navier-Stokes computational method is applied for analyzing the hydrodynamic heave response of the absorber in operational wave conditions. The two-body floating wave absorber contains a float section and a submerged reaction section. For validation purposes, our model is first assumed to be locked. The two sections are forced to move together with each other. The locked single body model is used in a heave decay test, where the RANS result is validated with the experimental measurement. For the two-body floating point absorber simulation, the two sections are connected through a mass-spring-damper system, which is applied to simulate the power take-off mechanism under design wave conditions. Overall, the details of the flow around the absorber and its nonlinear interaction with waves are investigated, and the power absorption efficiency of the two-body floating wave absorber in waves with a constant value spring-damper system is examined.

  3. An Operand-Optimized Asynchronous IEEE 754 Double-Precision Floating-Point Adder

    E-Print Network [OSTI]

    Manohar, Rajit

    a number of different data-dependent optimizations for energy-efficiency. Our baseline asynchronous FPA has of nonzero operands, our optimizations improve the FPA's energy-efficiency to 30.2 pJ per operation while, this performance is limited by power con- straints. The Top 500 supercomputer ranking now includes the energy-efficiency

  4. A rapid-approximation floating-point mathematics package for the INTEL 8080 microprocessor

    E-Print Network [OSTI]

    Cariker, Earnest Allan

    1981-01-01T23:59:59.000Z

    normalization Numeric stora e convention 2. 3 Mathematical Functions Review of lo arithmic theor Multi lication Division Addition Subtraction 12 12 13 13 15 16 17 17 ~St Tri onometric functions 2. 4 Computational Performance Re resentation... viii LIST OF FIGURES Figure B-II-1. Figure B-II-2. Figure B-II-3. Figure B-II-4. Figure B-II-5. Figure B-II-6. Figure B-II-7. Figure B-II-8. Program CONVL ? BCD to logarithmic format number conversion Program LGBCD ? logarithmic format...

  5. Design of a new compact and regular 8 x 8 multiplier using redundant binary number representation 

    E-Print Network [OSTI]

    Gopalan, Mythili

    1992-01-01T23:59:59.000Z

    . The n-bit multiplication time of the multiplier is proportional to logan. A modified redundant to binary converter is proposed. This resulted in a reduction of the delay time and the number of transistors of the multiplier. The multiplier adopted a.... The 8 x 8 multiplier was designed and simulated with both the converters. The modified converter reduced the delay time by 13. 7%, area by 33. 69% and number of transistors by 12. 9%. Estimates of area and speed for longer word lengths(16 x 16 and 32...

  6. Construction of Oscillating Chemical Register Machines on Binary Numbers using Mass-Action Kinetics

    E-Print Network [OSTI]

    Hinze, Thomas

    of computation for controlling continuous species concentrations enhances the applicability of both modelling of three natural numbers illustrates the practicability of the design. 1 Introduction For more than 20 lead to error-prone computations [13]. We introduce a mod- ular design principle for pure chemical

  7. Astrophysics of white dwarf binaries

    E-Print Network [OSTI]

    G. Nelemans

    2007-03-13T23:59:59.000Z

    White dwarf binaries are the most common compact binaries in the Universe and are especially important for low-frequency gravitational wave detectors such as LISA. There are a number of open questions about binary evolution and the Galactic population of white dwarf binaries that can be solved using gravitational wave data and at the same time, our ever improving knowledge about these binaries will help to predict the signals that can be expected for LISA. In addition a number of white dwarf binaries will serve as verification sources for the instrument. I will discuss these issues and report recent, surprising, developments in this field. Finally I report calculations about the feasibility of complementary electro-magnetic observations which unfortunately cannot reproduce the optimistic results of Cooray et al. (2004).

  8. Strategies for sharing a floating point unit between SPEs

    E-Print Network [OSTI]

    Lugo Martinez, Jose E.

    2010-01-01T23:59:59.000Z

    a proper balance between area, energy and performance for aper SPEs complex reduces area, energy and energy delay withis a tradeoff between area, energy and performance aspects

  9. L9: Next Assignment, Project and Floating Point

    E-Print Network [OSTI]

    Hall, Mary W.

    using GPU - Kannan Venkataraju, Mark Kim, Dan Gerszewski, James R. Anderson, and Mary Hall ­ Paper: GPU, Tyler Prete, Kevin Tew, Mary Hall, Phil Wallstedt, and James Guilkey · Poster at NVIDIA Research Summit

  10. L9: Next Assignment, Project and Floating Point

    E-Print Network [OSTI]

    Hall, Mary W.

    Images using GPU - Kannan Venkataraju, Mark Kim, Dan Gerszewski, James R. Anderson, and Mary Hall ­ PaperLisi, Todd Hummel, Tyler Prete, Kevin Tew, Mary Hall, Phil Wallstedt, and James Guilkey · Poster at NVIDIA

  11. Eclipsing Binaries in the Young LMC Cluster NGC 1850

    E-Print Network [OSTI]

    Stuart F. Taylor

    2004-10-21T23:59:59.000Z

    I present light curves for two detached eclipsing binary stars in the region of the LMC cluster NGC 1850, which is possibly a young globular cluster still in formation. One, a likely spectral type O star, is a newly detected eclipsing binary in the region of the very young subcluster NGC 1850A. This binary is among a small number of highly massive O-type stars in binary systems found in LMC clusters. These two eclipsing binaries are the first discovered in the well studied NGC 1850, and the O-type star is the first eclisping binary found in NGC 1850A. Light curves for two NGC 1850 region Cepheid variables are also shown. Discovering two eclipsing binaries in the young globlular-like cluster NGC 1850 is discussed in terms of the importance of the binary fraction to globular cluster evolution.

  12. THE ELM SURVEY. V. MERGING MASSIVE WHITE DWARF BINARIES

    SciTech Connect (OSTI)

    Brown, Warren R.; Kenyon, Scott J. [Smithsonian Astrophysical Observatory, 60 Garden St, Cambridge, MA 02138 (United States); Kilic, Mukremin; Gianninas, A. [Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks St., Norman, OK, 73019 (United States); Allende Prieto, Carlos, E-mail: wbrown@cfa.harvard.edu, E-mail: skenyon@cfa.harvard.edu, E-mail: kilic@ou.edu, E-mail: alexg@nhn.ou.edu, E-mail: callende@iac.es [Instituto de Astrofisica de Canarias, E-38205, La Laguna, Tenerife (Spain)

    2013-05-20T23:59:59.000Z

    We present the discovery of 17 low-mass white dwarfs (WDs) in short-period (P {<=} 1 day) binaries. Our sample includes four objects with remarkable log g {approx_equal} 5 surface gravities and orbital solutions that require them to be double degenerate binaries. All of the lowest surface gravity WDs have metal lines in their spectra implying long gravitational settling times or ongoing accretion. Notably, six of the WDs in our sample have binary merger times <10 Gyr. Four have {approx}>0.9 M{sub Sun} companions. If the companions are massive WDs, these four binaries will evolve into stable mass transfer AM CVn systems and possibly explode as underluminous supernovae. If the companions are neutron stars, then these may be millisecond pulsar binaries. These discoveries increase the number of detached, double degenerate binaries in the ELM Survey to 54; 31 of these binaries will merge within a Hubble time.

  13. 230.ps.gz

    E-Print Network [OSTI]

    Acknowledgement. I thank Bob Fourer for helpful comments on the manuscript. 9 References. IEEE Standard for Binary Floating-Point Arithmetic, Institute of ...

  14. The Ratio of Retrograde to Prograde Orbits: A Test for Kuiper Belt Binary Formation Theories

    E-Print Network [OSTI]

    Hilke E. Schlichting; Re'em Sari

    2008-07-03T23:59:59.000Z

    With the discovery of Kuiper Belt binaries that have wide separations and roughly equal masses new theories were proposed to explain their formation. Two formation scenarios were suggested by Goldreich and collaborators: In the first, dynamical friction that is generated by a sea of small bodies enables a transient binary to become bound ($L^2s$ mechanism); in the second, a transient binary gets bound by an encounter with a third body ($L^3$ mechanism). We show that these different binary formation scenarios leave their own unique signatures in the relative abundance of prograde to retrograde binary orbits. This signature is due to stable retrograde orbits that exist much further out in the Hill sphere than prograde orbits. It provides an excellent opportunity to distinguish between the different binary formation scenarios observationally. We predict that if binary formation proceeded while sub-Hill velocities prevailed, the vast majority of all comparable mass ratio binaries have retrograde orbits. This dominance of retrograde binary orbits is a result of binary formation via the $L^2s$ mechanism, or any other mechanism that dissipates energy in a smooth and gradual manner. For super-Hill velocities binary formation proceeds via the $L^3$ mechanism which produces a roughly equal number of prograde and retrograde binaries. These predictions assume that subsequent orbital evolution due to dynamical friction and dynamical stirring of the Kuiper belt did not alter the sense of the binary orbit after formation.

  15. The Binary Zoo: The Calculation of Production Rates of Binaries Through 2+1 Encounters in Globular Clusters

    E-Print Network [OSTI]

    M. B. Davies

    1995-07-07T23:59:59.000Z

    In studying encounters between binaries and single stars, one is interested in three classes of events: exchanges of stars, hardening of the original binary by a third star, and the production of merged objects. We present a means for computing cross sections for these three outcomes for an arbitrary binary and single star as might be found in the core of a globular cluster. The cross sections for a number of binaries in various stellar populations are then computed. We consider multiple encounters and the ultimate fate of a population of binaries fed into the cores of different globular cluster models. We see that the presence of only a relatively small number of binaries (containing 10\\% of the stars) will boost the production rate of astrophysically-interesting objects by a factor of at least a few over the rates expected from encounters between single stars. In particular, the ratio of smothered neutron stars to low-mass X-ray binaries (LMXBs) may be greatly increased, possibly explaining, in part, the excess of millisecond pulsars compared to LMXBs.

  16. Binary power multiplier for electromagnetic energy

    DOE Patents [OSTI]

    Farkas, Zoltan D. (203 Leland Ave., Menlo Park, CA 94025)

    1988-01-01T23:59:59.000Z

    A technique for converting electromagnetic pulses to higher power amplitude and shorter duration, in binary multiples, splits an input pulse into two channels, and subjects the pulses in the two channels to a number of binary pulse compression operations. Each pulse compression operation entails combining the pulses in both input channels and selectively steering the combined power to one output channel during the leading half of the pulses and to the other output channel during the trailing half of the pulses, and then delaying the pulse in the first output channel by an amount equal to half the initial pulse duration. Apparatus for carrying out each of the binary multiplication operation preferably includes a four-port coupler (such as a 3 dB hybrid), which operates on power inputs at a pair of input ports by directing the combined power to either of a pair of output ports, depending on the relative phase of the inputs. Therefore, by appropriately phase coding the pulses prior to any of the pulse compression stages, the entire pulse compression (with associated binary power multiplication) can be carried out solely with passive elements.

  17. Area-Efficient Evaluation of Arithmetic Expressions Using Deeply Pipelined Floating-Point Cores1

    E-Print Network [OSTI]

    Prasanna, Viktor K.

    of such expressions must be evaluated in molecular dynamics simulations, for example. Such expressions usually have of Electrical Engineering University of Southern California Los Angeles, CA¢ rscrofan, lzhuo, prasanna£ @usc

  18. Ultra-Low-Power Adder Stage Design for Exascale Floating Point Units

    E-Print Network [OSTI]

    Del Barrio, AA; Bagherzadeh, N; Hermida, R

    2014-01-01T23:59:59.000Z

    date: March 2014. Ultra-Low-Power Adder Stage Design fordate: March 2014. Ultra-Low-Power Adder Stage Design fordate: March 2014. Ultra-Low-Power Adder Stage Design for

  19. Experimental Wave Tank Test for Reference Model 3 Floating-Point Absorber Wave Energy Converter Project

    SciTech Connect (OSTI)

    Yu, Y. H.; Lawson, M.; Li, Y.; Previsic, M.; Epler, J.; Lou, J.

    2015-01-01T23:59:59.000Z

    The U.S. Department of Energy established a reference model project to benchmark a set of marine and hydrokinetic technologies including current (tidal, open-ocean, and river) turbines and wave energy converters. The objectives of the project were to first evaluate the status of these technologies and their readiness for commercial applications. Second, to evaluate the potential cost of energy and identify cost-reduction pathways and areas where additional research could be best applied to accelerate technology development to market readiness.

  20. Low-Power Single-Precision IEEE Floating-Point Sheetal A. Jain

    E-Print Network [OSTI]

    Asanovi?, Krste

    adder with and without inhibit control and the single path adder, to determine the most energy efficient design. Thesis Supervisor: Krste Asanovic Title: Assistant Professor 3 #12;4 #12;Acknowledgments I would

  1. A study of some methods of numerical integration using floating point arithmetic

    E-Print Network [OSTI]

    Young, John Mackay

    1959-01-01T23:59:59.000Z

    IN NUMERICAL INTEGRATION e ~ ~ e ~ ~ ~ ~ ~ e EVALUATION OF A FRESNEL INTEGRAL AS A POWER SERIES EXPANSION a ~ ~ o ~ ~ ~ ~ ~ DISCUSSIOM OF TWO MAJOR SOURCES OF ERROR WHEN INTEGRATING USING FLOATIMG POINT ARITHNEPICa e ~ ~ a ~ ~ e ~ ~ ~ ~ e ~ ~ ~ ~ 13 V...(x) ~ 10 for 0 c x c 10 f(x) = -10x + 110 for 10 c x c 11 ))0 c x c, 85 One of the Fresnel integrals was chosen because the Fresnel integrals are interesting to physicists as well as mathematicians. It was used only in the study of numerical...

  2. Experimental Wave Tank Test for Reference Model 3 Floating-Point Absorber Wave Energy Converter Project

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOEThe Bonneville Power AdministrationField8,Dist. Category UC-l 1,Energy ConsumersExperimental Test ofExperimental

  3. Accretion in Compact Binaries

    E-Print Network [OSTI]

    Andrew R. King

    2003-03-26T23:59:59.000Z

    Compact binaries have long been a paradigm for accretion theory. Much of our present view of how accretion occurs comes directly from the comparison of theory with observations of these sources. Since theory differs little for other objects such as active galaxies, increasing efforts have recently gone into searching for correspondences in observed behaviour. This chapter aims at giving a concise summary of the field, with particular emphasis on new developments since the previous edition of this book. These developments have been significant. Much of the earlier literature implicitly assumed that accreting binaries were fairly steady sources accreting most of the mass entering their vicinity, often with main-sequence companions, and radiating the resulting accretion luminosity in rough isotropy. We shall see that in reality these assumptions fail for the majority of systems. Most are transient; mass ejection in winds and jets is extremely common; a large (sometimes dominant) fraction of even short-period systems have evolved companions whose structure deviates significantly from the zero-age main sequence; and the radiation pattern of many objects is significantly anisotropic. It is now possible to give a complete characterization of the observed incidence of transient and persistent sources in terms of the disc instability model and formation constraints. X-ray populations in external galaxies, particularly the ultraluminous sources, are revealing important new insights into accretion processes and compact binary evolution.

  4. High-resolution radio observations of X-ray binaries

    E-Print Network [OSTI]

    James Miller-Jones

    2008-09-15T23:59:59.000Z

    I present an overview of important results obtained using high-resolution very long baseline interferometry (VLBI) observations of X-ray binary systems. These results derive from both astrometric observations and resolved imaging of sources, from black holes to neutron star and even white dwarf systems. I outline a number of upcoming developments in instrumentation, both new facilities and ongoing upgrades to existing VLBI instruments, and I conclude by identifying a number of important areas of investigation where VLBI will be crucial in advancing our understanding of X-ray binaries.

  5. Dynamic Tides in Close Binaries

    E-Print Network [OSTI]

    B. Willems

    2005-11-10T23:59:59.000Z

    The basic theory of dynamic tides in close binaries is reviewed. Particular attention is paid to resonances between dynamic tides and free oscillation modes and to the role of the apsidal-motion rate in probing the internal structure of binary components. The discussed effects are generally applicable to stars across the entire Hertzsprung-Russell diagram, including the binary OB-stars discussed at this meeting.

  6. Chaos in Binary Category Computation

    E-Print Network [OSTI]

    Carlos Pedro Gonçalves

    2010-11-21T23:59:59.000Z

    Category computation theory deals with a web-based systemic processing that underlies the morphic webs, which constitute the basis of categorial logical calculus. It is proven that, for these structures, algorithmically incompressible binary patterns can be morphically compressed, with respect to the local connectivities, in a binary morphic program. From the local connectivites, there emerges a global morphic connection that can be characterized by a low length binary string, leading to the identification of chaotic categorial dynamics, underlying the algorithmically random pattern. The work focuses on infinite binary chains of C2, which is a category that implements an X-OR-based categorial logical calculus.

  7. IntrAst2 (Petrovay) Binaries BINARY STARS

    E-Print Network [OSTI]

    Petrovay, Kristóf

    ;IntrAst2 (Petrovay) Binaries The Doppler effect and stellar radial velocities Moving wave source / = /c : recession velocity of source; c: wave propagation speed (for c) Radial velocities of nearby) Spectroscopic binaries Periodic wavelength shifts in spectral lines due to orbital motion (Doppler shifts). #12

  8. Beowawe Binary Bottoming Cycle

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels DataDepartment of Energy Your Density Isn't Your Destiny: The FutureCommentsEnergy Christopher| Department ofBeowawe Binary Bottoming

  9. Binary Frequencies in Globular Clusters

    E-Print Network [OSTI]

    Ji, Jun

    2015-01-01T23:59:59.000Z

    Binary stars are predicted to have an important role in the evolution of globular clusters, so we obtained binary fractions for 35 globular clusters that were imaged in the F606W and F814W with the ACS on the Hubble Space Telescope. When compared to the values of prior efforts (Sollima et al. 2007; Milone et al. 2012), we find significant discrepancies, despite each group correcting for contamination effects and having performed the appropriate reliability tests. The most reliable binary fractions are obtained when restricting the binary fraction to q > 0.5. Our analysis indicates that the range of the binary fractions is nearly an order of magnitude for the lowest dynamical ages, suggesting that there is a broad distribution in the binary fraction at globular cluster formation. Dynamical effects also appears to decrease the core binary fractions by a factor of two over a Hubble time, but this is a weak relationship. We confirm a correlation from previous work that the binary fraction within the core radius d...

  10. Spectroscopic Binary Mass Determination using Relativity

    E-Print Network [OSTI]

    Zucker, S; Zucker, Shay; Alexander, Tal

    2006-01-01T23:59:59.000Z

    High-precision radial-velocity techniques, which enabled the detection of extrasolar planets are now sensitive to relativistic effects in the data of spectroscopic binary stars (SBs). We show how these effects can be used to derive the absolute masses of the components of eclipsing single-lined SBs and double-lined SBs from Doppler measurements alone. High-precision stellar spectroscopy can thus substantially increase the number of measured sellar masses, thereby improving the mass-radius and mass-magnitude calibrations.

  11. Spectroscopic Binary Mass Determination using Relativity

    E-Print Network [OSTI]

    Shay Zucker; Tal Alexander

    2006-11-14T23:59:59.000Z

    High-precision radial-velocity techniques, which enabled the detection of extrasolar planets are now sensitive to relativistic effects in the data of spectroscopic binary stars (SBs). We show how these effects can be used to derive the absolute masses of the components of eclipsing single-lined SBs and double-lined SBs from Doppler measurements alone. High-precision stellar spectroscopy can thus substantially increase the number of measured stellar masses, thereby improving the mass-radius and mass-luminosity calibrations.

  12. Lifting Integrity Constraints in Binary Aggregation Umberto Grandi

    E-Print Network [OSTI]

    Endriss, Ulle

    Lifting Integrity Constraints in Binary Aggregation Umberto Grandi and Ulle Endriss Institute language and we explore the question of whether or not a given aggregation procedure will lift a given, this discipline has received increasing attention in Artificial Intelligence (AI), as testified by a large number

  13. Optimization Methods for Binary Sequences The Merit Factor Problem

    E-Print Network [OSTI]

    Optimization Methods for Binary Sequences ­ The Merit Factor Problem Ron Ferguson, Joshua Knauer SFU MOCAA Project Leader: Peter Borwein MITACS 6th Annual Conference, May, 2005 Abstract Optimization of much interest in combinatorial optimization, communications engineering, and analytic number theory

  14. accurate multiple locus: Topics by E-print Network

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    severe economic losses in the main apple producing areas of East Asia. The causal Biggs, Alan R. 8 Accurate Matrix Multiplication with Multiple Floating-point Numbers...

  15. Training a Binary Classifier with the Quantum Adiabatic Algorithm

    E-Print Network [OSTI]

    Hartmut Neven; Vasil S. Denchev; Geordie Rose; William G. Macready

    2008-11-04T23:59:59.000Z

    This paper describes how to make the problem of binary classification amenable to quantum computing. A formulation is employed in which the binary classifier is constructed as a thresholded linear superposition of a set of weak classifiers. The weights in the superposition are optimized in a learning process that strives to minimize the training error as well as the number of weak classifiers used. No efficient solution to this problem is known. To bring it into a format that allows the application of adiabatic quantum computing (AQC), we first show that the bit-precision with which the weights need to be represented only grows logarithmically with the ratio of the number of training examples to the number of weak classifiers. This allows to effectively formulate the training process as a binary optimization problem. Solving it with heuristic solvers such as tabu search, we find that the resulting classifier outperforms a widely used state-of-the-art method, AdaBoost, on a variety of benchmark problems. Moreover, we discovered the interesting fact that bit-constrained learning machines often exhibit lower generalization error rates. Changing the loss function that measures the training error from 0-1 loss to least squares maps the training to quadratic unconstrained binary optimization. This corresponds to the format required by D-Wave's implementation of AQC. Simulations with heuristic solvers again yield results better than those obtained with boosting approaches. Since the resulting quadratic binary program is NP-hard, additional gains can be expected from applying the actual quantum processor.

  16. Relaxation dynamics in a binary hard-ellipse liquid

    E-Print Network [OSTI]

    Wen-Sheng Xu; Zhao-Yan Sun; Li-Jia An

    2014-12-01T23:59:59.000Z

    Structural relaxation in binary hard spherical particles has been shown recently to exhibit a wealth of remarkable features when size disparity or mixture's composition is varied. In this paper, we test whether or not similar dynamical phenomena occur in glassy systems composed of binary hard ellipses. We demonstrate via event-driven molecular dynamics simulation that a binary hard-ellipse mixture with an aspect ratio of two and moderate size disparity displays characteristic glassy dynamics upon increasing density in both the translational and the rotational degrees of freedom. The rotational glass transition density is found to be close to the translational one for the binary mixtures investigated. More importantly, we assess the influence of size disparity and mixture's composition on the relaxation dynamics. We find that an increase of size disparity leads, both translationally and rotationally, to a speed up of the long-time dynamics in the supercooled regime so that both the translational and the rotational glass transition shift to higher densities. By increasing the number concentration of the small particles, the time evolution of both translational and rotational relaxation dynamics at high densities displays two qualitatively different scenarios, i.e., both the initial and the final part of the structural relaxation slow down for small size disparity, while the short-time dynamics still slows down but the final decay speeds up in the binary mixture with large size disparity. These findings are reminiscent of those observed in binary hard spherical particles. Therefore, our results suggest a universal mechanism for the influence of size disparity and mixture's composition on the structural relaxation in both isotropic and anisotropic particle systems.

  17. Spectral analysis of X-ray binaries

    E-Print Network [OSTI]

    Fridriksson, Joel Karl

    2011-01-01T23:59:59.000Z

    In this thesis, I present work from three separate research projects associated with observations of X-ray binaries. Two of those revolve around spectral characteristics of neutron star low-mass X-ray binaries (NS-LMXBs), ...

  18. Permanent Home Number: Residential Number

    E-Print Network [OSTI]

    Viglas, Anastasios

    Permanent Home Number: Residential Number: Mobile: Please update my contact details. Signature nominated correspondence address as indicated below. Permanent Home Adress Residential Address Other Address (Must not be a PO Box) Residential Address (Must not be a PO Box) Other - Postal/Optional Address

  19. UNIT NUMBER:

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    193 UNIT NUMBER: 197 UNIT NAME: CONCRETE RUBBLE PILE (30) REGULATORY STATUS: AOC LOCATION: Outside plant security fence, north of the plant on Big Bayou Creek on private property....

  20. T-694: IBM Tivoli Federated Identity Manager Products Multiple Vulnerabilities

    Broader source: Energy.gov [DOE]

    This Security Alert addresses a serious security issue CVE-2010-4476 (Java Runtime Environment hangs when converting "2.2250738585072012e-308" to a binary floating-point number). This vulnerability might cause the Java Runtime Environment to hang, be in infinite loop, and/or crash resulting in a denial of service exposure. This same hang might occur if the number is written without scientific notation (324 decimal places). In addition to the Application Server being exposed to this attack, any Java program using the Double.parseDouble method is also at risk of this exposure including any customer written application or third party written application.

  1. Merger of white dwarf-neutron star binaries: Prelude to hydrodynamic simulations in general relativity

    SciTech Connect (OSTI)

    Paschalidis, Vasileios [Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801 (United States); MacLeod, Morgan [Department of Physics and Astronomy, Bowdoin College, Brunswick, Maine 04011 (United States); Baumgarte, Thomas W. [Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801 (United States); Department of Physics and Astronomy, Bowdoin College, Brunswick, Maine 04011 (United States); Shapiro, Stuart L. [Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801 (United States); Department of Astronomy and NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801 (United States)

    2009-07-15T23:59:59.000Z

    White dwarf-neutron star binaries generate detectable gravitational radiation. We construct Newtonian equilibrium models of corotational white dwarf-neutron star (WDNS) binaries in circular orbit and find that these models terminate at the Roche limit. At this point the binary will undergo either stable mass transfer (SMT) and evolve on a secular time scale, or unstable mass transfer (UMT), which results in the tidal disruption of the WD. The path a given binary will follow depends primarily on its mass ratio. We analyze the fate of known WDNS binaries and use population synthesis results to estimate the number of LISA-resolved galactic binaries that will undergo either SMT or UMT. We model the quasistationary SMT epoch by solving a set of simple ordinary differential equations and compute the corresponding gravitational waveforms. Finally, we discuss in general terms the possible fate of binaries that undergo UMT and construct approximate Newtonian equilibrium configurations of merged WDNS remnants. We use these configurations to assess plausible outcomes of our future, fully relativistic simulations of these systems. If sufficient WD debris lands on the NS, the remnant may collapse, whereby the gravitational waves from the inspiral, merger, and collapse phases will sweep from LISA through LIGO frequency bands. If the debris forms a disk about the NS, it may fragment and form planets.

  2. LONG-TERM STABLE EQUILIBRIA FOR SYNCHRONOUS BINARY ASTEROIDS

    SciTech Connect (OSTI)

    Jacobson, Seth A. [Department of Astrophysical and Planetary Sciences, University of Colorado at Boulder, Boulder, CO 80309 (United States); Scheeres, Daniel J. [Department of Aerospace Engineering Sciences, University of Colorado at Boulder, Boulder, CO 80309 (United States)

    2011-07-20T23:59:59.000Z

    Synchronous binary asteroids may exist in a long-term stable equilibrium, where the opposing torques from mutual body tides and the binary YORP (BYORP) effect cancel. Interior of this equilibrium, mutual body tides are stronger than the BYORP effect and the mutual orbit semimajor axis expands to the equilibrium; outside of the equilibrium, the BYORP effect dominates the evolution and the system semimajor axis will contract to the equilibrium. If the observed population of small (0.1-10 km diameter) synchronous binaries are in static configurations that are no longer evolving, then this would be confirmed by a null result in the observational tests for the BYORP effect. The confirmed existence of this equilibrium combined with a shape model of the secondary of the system enables the direct study of asteroid geophysics through the tidal theory. The observed synchronous asteroid population cannot exist in this equilibrium if described by the canonical 'monolithic' geophysical model. The 'rubble pile' geophysical model proposed by Goldreich and Sari is sufficient, however it predicts a tidal Love number directly proportional to the radius of the asteroid, while the best fit to the data predicts a tidal Love number inversely proportional to the radius. This deviation from the canonical and Goldreich and Sari models motivates future study of asteroid geophysics. Ongoing BYORP detection campaigns will determine whether these systems are in an equilibrium, and future determination of secondary shapes will allow direct determination of asteroid geophysical parameters.

  3. Bayesian decision making in human collectives with binary choices

    E-Print Network [OSTI]

    Eguíluz, Víctor M; Fernández-Gracia, J

    2015-01-01T23:59:59.000Z

    Here we focus on the description of the mechanisms behind the process of information aggregation and decision making, a basic step to understand emergent phenomena in society, such as trends, information spreading or the wisdom of crowds. In many situations, agents choose between discrete options. We analyze experimental data on binary opinion choices in humans. The data consists of two separate experiments in which humans answer questions with a binary response, where one is correct and the other is incorrect. The questions are answered without and with information on the answers of some previous participants. We find that a Bayesian approach captures the probability of choosing one of the answers. The influence of peers is uncorrelated with the difficulty of the question. The data is inconsistent with Weber's law, which states that the probability of choosing an option depends on the proportion of previous answers choosing that option and not on the total number of those answers. Last, the present Bayesian ...

  4. Compact binary mergers: an astrophysical perspective

    E-Print Network [OSTI]

    S. Rosswog

    2010-12-22T23:59:59.000Z

    This paper reviews the current understanding of double neutron star and neutron star black hole binaries. It addresses mainly (nuclear) astrophysics aspects of compact binary mergers and thus complements recent reviews that have emphasized the numerical relativity viewpoint. In particular, the paper discusses different channels to release neutron-rich matter into the host galaxy, connections between compact binary mergers and short Gamma-ray bursts and accompanying electromagnetic signals.

  5. Change Number

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645 3,625govInstrumentstdmadapInactiveVisiting the TWPSuccessAlamos LaboratoryCertified Reference6-02-01Change Number

  6. Approximate initial data for binary black holes

    E-Print Network [OSTI]

    Kenneth A. Dennison; Thomas W. Baumgarte; Harald P. Pfeiffer

    2006-08-26T23:59:59.000Z

    We construct approximate analytical solutions to the constraint equations of general relativity for binary black holes of arbitrary mass ratio in quasicircular orbit. We adopt the puncture method to solve the constraint equations in the transverse-traceless decomposition and consider perturbations of Schwarzschild black holes caused by boosts and the presence of a binary companion. A superposition of these two perturbations then yields approximate, but fully analytic binary black hole initial data that are accurate to first order in the inverse of the binary separation and the square of the black holes' momenta.

  7. NONLINEAR TIDES IN CLOSE BINARY SYSTEMS

    SciTech Connect (OSTI)

    Weinberg, Nevin N. [Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139 (United States); Arras, Phil [Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325 (United States); Quataert, Eliot; Burkart, Josh, E-mail: nevin@mit.edu [Astronomy Department and Theoretical Astrophysics Center, 601 Campbell Hall, University of California, Berkeley, CA 94720 (United States)

    2012-06-01T23:59:59.000Z

    We study the excitation and damping of tides in close binary systems, accounting for the leading-order nonlinear corrections to linear tidal theory. These nonlinear corrections include two distinct physical effects: three-mode nonlinear interactions, i.e., the redistribution of energy among stellar modes of oscillation, and nonlinear excitation of stellar normal modes by the time-varying gravitational potential of the companion. This paper, the first in a series, presents the formalism for studying nonlinear tides and studies the nonlinear stability of the linear tidal flow. Although the formalism we present is applicable to binaries containing stars, planets, and/or compact objects, we focus on non-rotating solar-type stars with stellar or planetary companions. Our primary results include the following: (1) The linear tidal solution almost universally used in studies of binary evolution is unstable over much of the parameter space in which it is employed. More specifically, resonantly excited internal gravity waves in solar-type stars are nonlinearly unstable to parametric resonance for companion masses M' {approx}> 10-100 M{sub Circled-Plus} at orbital periods P Almost-Equal-To 1-10 days. The nearly static 'equilibrium' tidal distortion is, however, stable to parametric resonance except for solar binaries with P {approx}< 2-5 days. (2) For companion masses larger than a few Jupiter masses, the dynamical tide causes short length scale waves to grow so rapidly that they must be treated as traveling waves, rather than standing waves. (3) We show that the global three-wave treatment of parametric instability typically used in the astrophysics literature does not yield the fastest-growing daughter modes or instability threshold in many cases. We find a form of parametric instability in which a single parent wave excites a very large number of daughter waves (N Almost-Equal-To 10{sup 3}[P/10 days] for a solar-type star) and drives them as a single coherent unit with growth rates that are a factor of Almost-Equal-To N faster than the standard three-wave parametric instability. These are local instabilities viewed through the lens of global analysis; the coherent global growth rate follows local rates in the regions where the shear is strongest. In solar-type stars, the dynamical tide is unstable to this collective version of the parametric instability for even sub-Jupiter companion masses with P {approx}< a month. (4) Independent of the parametric instability, the dynamical and equilibrium tides excite a wide range of stellar p-modes and g-modes by nonlinear inhomogeneous forcing; this coupling appears particularly efficient at draining energy out of the dynamical tide and may be more important than either wave breaking or parametric resonance at determining the nonlinear dissipation of the dynamical tide.

  8. *PHDD: An Efficient Graph Representation for Floating Point Circuit Verification y YirngAn Chen Randal E. Bryant

    E-Print Network [OSTI]

    Bryant, Randal E.

    Randal E. Bryant yachen@cs.cmu.edu Randy.Bryant@cs.cmu.edu Carnegie Mellon University, Pittsburgh, PA

  9. *PHDD: An Efficient Graph Representation for Floating Point Circuit Verification Yirng-An Chen Randal E. Bryant

    E-Print Network [OSTI]

    Bryant, Randal E.

    Randal E. Bryant yachen@cs.cmu.edu Randy.Bryant@cs.cmu.edu Carnegie Mellon University, Pittsburgh, PA

  10. Profligate Execution Nearly four decades after its first implementation in the IBM 360/91 floating-point

    E-Print Network [OSTI]

    Lipasti, Mikko H.

    . Diminishing performance returns and the difficulty of building large, monolithic instruction windows has of transistors that can fit on a single chip as well as the decreasing distance that a signal can travel that obtains comparable performance to a single monolithic window. As with many tech- niques that attempt

  11. Impact flux of asteroids and water transport to the habitable zone in binary star systems

    E-Print Network [OSTI]

    Bancelin, D; Eggl, S; Dvorak, R

    2015-01-01T23:59:59.000Z

    By now, observations of exoplanets have found more than 50 binary star systems hosting 71 planets. We expect these numbers to increase as more than 70% of the main sequence stars in the solar neighborhood are members of binary or multiple systems. The planetary motion in such systems depends strongly on both the parameters of the stellar system (stellar separation and eccentricity) and the architecture of the planetary system (number of planets and their orbital behaviour). In case a terrestrial planet moves in the so-called habitable zone (HZ) of its host star, the habitability of this planet depends on many parameters. A crucial factor is certainly the amount of water. We investigate in this work the transport of water from beyond the snow-line to the HZ in a binary star system and compare it to a single star system.

  12. Evolution of Compact-Binary Populations in Globular Clusters: A Boltzmann Study. I. The Continuous Limit

    E-Print Network [OSTI]

    Sambaran Banerjee; Pranab Ghosh

    2007-08-10T23:59:59.000Z

    We explore a Boltzmann scheme for studying the evolution of compact binary populations of globular clusters. We include processes of compact-binary formation by tidal capture and exchange encounters, binary destruction by dissociation and other mechanisms, and binary hardening by encounters, gravitational radiation and magnetic braking, as also the orbital evolution during mass transfer, following Roche lobe contact. For the encounter processes which are stochastic in nature, we study the probabilistic, continuous limit in this introductory work, deferring the specific handling of the stochastic terms to the next step. We focus on the evolution of (a) the number of X-ray sources N_{XB} in globular clusters, and (b) the orbital-period distribution of the X-ray binaries, as a result of the above processes. We investigate the dependence of N_{XB} on two essential cluster properties, namely, the star-star and star-binary encounter-rate parameters 'Gamma' and 'gamma', which we call Verbunt parameters. We compare our model results with observation, showing that the model values of N_{XB} and their expected scaling with the Verbunt parameters are in good agreement with results from recent X-ray observations of Galactic globular clusters, encouraging us to build more detailed models.

  13. The Evolution of Compact Binary Star Systems

    E-Print Network [OSTI]

    Konstantin Postnov; Lev Yungelson

    2014-03-21T23:59:59.000Z

    We review the formation and evolution of compact binary stars consisting of white dwarfs (WDs), neutron stars (NSs), and black holes (BHs). Mergings of compact binary stars are expected to be the most important sources for the forthcoming gravitational-wave (GW) astronomy. In the first part of the review, we discuss observational manifestations of close binary stars with NS and/or black components and their merger rate, crucial points in the formation and evolution of compact stars in binary systems, including the treatment of the natal kicks which NSs and BHs acquire during the core collapse of massive stars and the common envelope phase of binary evolution, which are most relevant to the merging rates of NS-NS, NS-BH and BH-BH binaries. The second part of the review is devoted mainly to formation and evolution of binary WDs and their observational manifestations, including their role as progenitors of cosmologically important thermonuclear SN Ia. We also consider AM CVn-stars which are thought to be the best verification binary GW sources for future low-frequency GW space interferometers.

  14. The apsidal motion in close binary stars

    E-Print Network [OSTI]

    B. V. Vasiliev

    2001-10-10T23:59:59.000Z

    It is usually accepted to consider an apsidal motion in binary stars as a direct confirmation that a substance inside stars is not uniformly distributed. It is shown in this paper that the apsidal motion in binary systems observation data is in a good agreement with an existence of uniform plasma cores inside stars if they consist of hydrogen-deuterium-helium mixture.

  15. Phase Transition in a Vlasov-Boltzmann Binary Mixture

    E-Print Network [OSTI]

    R. Esposito; Y. Guo; R. Marra

    2009-04-05T23:59:59.000Z

    There are not many kinetic models where it is possible to prove bifurcation phenomena for any value of the Knudsen number. Here we consider a binary mixture over a line with collisions and long range repulsive interaction between different species. It undergoes a segregation phase transition at sufficiently low temperature. The spatially homogeneous Maxwellian equilibrium corresponding to the mixed phase, minimizing the free energy at high temperature, changes into a maximizer when the temperature goes below a critical value, while non homogeneous minimizers, corresponding to coexisting segregated phases, arise. We prove that they are dynamically stable with respect to the Vlasov-Boltzmann evolution, while the homogeneous equilibrium becomes dynamically unstable.

  16. Electromagnetic Signatures of Massive Black Hole Binaries

    E-Print Network [OSTI]

    Tamara Bogdanovic; Britton D. Smith; Michael Eracleous; Steinn Sigurdsson

    2006-09-28T23:59:59.000Z

    We model the electromagnetic emission signatures of massive black hole binaries (MBHBs) with an associated gas component. The method comprises numerical simulations of relativistic binaries and gas coupled with calculations of the physical properties of the emitting gas. We calculate the accretion powered UV/X-ray and Halpha light curves and the Halpha emission line profiles. The simulations have been carried out with a modified version of the parallel tree SPH code Gadget. The heating, cooling, and radiative processes for the solar metallicity gas have been calculated with the photoionization code Cloudy. We investigate gravitationally bound, sub-parsec binaries which have not yet entered the gravitational radiation phase. The results from the first set of calculations, carried out for a coplanar binary and gas disk, suggest that the outbursts in the X-ray light curve are pronounced during pericentric passages and can serve as a fingerprint for this type of binaries if periodic outbursts are a long lived signature of the binary. The Halpha emission-line profiles also offer strong indications of a binary presence and may be used as a criterion for selection of MBHB candidates for further monitoring from existing archival data. The orbital period and mass ratio of a binary could be determined from the Halpha light curves and profiles of carefully monitored candidates. Although systems with the orbital periods studied here are not within the frequency band of the Laser Interferometer Space Antenna (LISA), their discovery is important for understanding of the merger rates of MBHBs and the evolution of such binaries through the last parsec and towards the detectable gravitational wave window.

  17. Distinguishing compact binary population synthesis models using gravitational-wave observations of coalescing binary black holes

    E-Print Network [OSTI]

    Stevenson, Simon; Fairhurst, Stephen

    2015-01-01T23:59:59.000Z

    The coalescence of compact binaries containing neutron stars or black holes is one of the most promising signals for advanced ground-based laser interferometer gravitational-wave detectors, with the first direct detections expected over the next few years. The rate of binary coalescences and the distribution of component masses is highly uncertain, and population synthesis models predict a wide range of plausible values. Poorly constrained parameters in population synthesis models correspond to poorly understood astrophysics at various stages in the evolution of massive binary stars, the progenitors of binary neutron star and binary black hole systems. These include effects such as supernova kick velocities, parameters governing the energetics of common envelope evolution and the strength of stellar winds. Observing multiple binary black hole systems through gravitational waves will allow us to infer details of the astrophysical mechanisms that lead to their formation. We simulate gravitational-wave observati...

  18. Microlensing Detections of Planets in Binary Stellar Systems

    E-Print Network [OSTI]

    Dong-Wook Lee; Chung-Uk Lee; Byeong-Gon Park; Sun-Ju Chung; Young-Soo Kim; Ho-Il Kim; Cheongho Han

    2007-09-13T23:59:59.000Z

    We demonstrate that microlensing can be used for detecting planets in binary stellar systems. This is possible because in the geometry of planetary binary systems where the planet orbits one of the binary component and the other binary star is located at a large distance, both planet and secondary companion produce perturbations at a common region around the planet-hosting binary star and thus the signatures of both planet and binary companion can be detected in the light curves of high-magnification lensing events. We find that identifying planets in binary systems is optimized when the secondary is located in a certain range which depends on the type of the planet. The proposed method can detect planets with masses down to one tenth of the Jupiter mass in binaries with separations planet mass and binary separation are not covered by other methods and thus microlensing would be able to make the planetary binary sample richer.

  19. Binary Tomography with Deblurring Stefan Weber1

    E-Print Network [OSTI]

    Schnörr, Christoph

    Binary Tomography with Deblurring Stefan Weber1 , Thomas Sch¨ule1,3 , Attila Kuba2 , and Christoph-Verlag Berlin Heidelberg 2006 #12;376 S. Weber et al. quality of the reconstructed images. The correction

  20. Photon transport in binary photonic lattices

    E-Print Network [OSTI]

    B. M. Rodríguez-Lara; H. Moya-Cessa

    2013-01-08T23:59:59.000Z

    We present a review on the mathematical methods used to theoretically study classical propagation and quantum transport in arrays of coupled photonic waveguides. We focus on analysing two types of binary photonic lattices where self-energies or couplings are alternated. For didactic reasons, we split the analysis in classical propagation and quantum transport but all methods can be implemented, mutatis mutandis, in any given case. On the classical side, we use coupled mode theory and present an operator approach to Floquet-Bloch theory in order to study the propagation of a classical electromagnetic field in two particular infinite binary lattices. On the quantum side, we study the transport of photons in equivalent finite and infinite binary lattices by couple mode theory and linear algebra methods involving orthogonal polynomials. Curiously the dynamics of finite size binary lattices can be expressed as roots and functions of Fibonacci polynomials.

  1. BAYESIAN RESIDUAL ANALYSIS FOR BINARY RESPONSE

    E-Print Network [OSTI]

    Albert, James H.

    of Mathematics and Statistics Bowling Green State University, Bowling Green, 43403 USA Siddhartha Chib Olin School of Business Washington University, St. Louis 63130 USA March, 1994 Summary In a binary response

  2. ROTATIONAL DOPPLER BEAMING IN ECLIPSING BINARIES

    SciTech Connect (OSTI)

    Groot, Paul J., E-mail: pgroot@astro.ru.nl [Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125 (United States)

    2012-01-20T23:59:59.000Z

    In eclipsing binaries the stellar rotation of the two components will cause a rotational Doppler beaming during eclipse ingress and egress when only part of the eclipsed component is covered. For eclipsing binaries with fast spinning components this photometric analog of the well-known spectroscopic Rossiter-McLaughlin effect can exceed the strength of the orbital effect. Example light curves are shown for a detached double white dwarf binary, a massive O-star binary and a transiting exoplanet case, similar to WASP-33b. Inclusion of the rotational Doppler beaming in eclipsing systems is a prerequisite for deriving the correct stellar parameters from fitting high-quality photometric light curves and can be used to determine stellar obliquities as well as, e.g., an independent measure of the rotational velocity in those systems that may be expected to be fully synchronized.

  3. Gravitational waves from merging compact binaries

    E-Print Network [OSTI]

    Hughes, Scott A.

    Largely motivated by the development of highly sensitive gravitational-wave detectors, our understanding of merging compact binaries and the gravitational waves they generate has improved dramatically in recent years. ...

  4. Blue Stragglers, Be stars and X-ray binaries in open clusters

    E-Print Network [OSTI]

    Amparo Marco; Ignacio Negueruela; Christian Motch

    2005-12-19T23:59:59.000Z

    Combination of high-precision photometry and spectroscopy allows the detailed study of the upper main sequence in open clusters. We are carrying out a comprehensive study of a number of clusters containing Be stars in order to evaluate the likelihood that a significant number of Be stars form through mass exchange in a binary. Our first results show that most young open clusters contain blue stragglers. In spite of the small number of clusters so far analysed, some trends are beginning to emerge. In younger open clusters, such as NGC 869 and NGC 663, there are many blue stragglers, most of which are not Be stars. In older clusters, such as IC 4725, the fraction of Be stars among blue stragglers is very high. Two Be blue stragglers are moderately strong X-ray sources, one of them being a confirmed X-ray binary. Such objects must have formed through binary evolution. We discuss the contribution of mass transfer in a close binary to the formation of both blue stragglers and Be stars

  5. Selection effects in resolving Galactic binaries with LISA

    E-Print Network [OSTI]

    M. J. Benacquista; S. L. Larson; B. E. Taylor

    2007-03-01T23:59:59.000Z

    Using several realisations of the Galactic population of close white dwarf binaries, we have explored the selection bias for resolved binaries in the LISA data stream. We have assumed a data analysis routine that is capable of identifying binaries that have a signal to noise ratio of at least 5 above a confusion foreground of unresolved binaries. The resolved population of binaries is separated into a subpopulation over 1000 binaries that have a measureable chirp and another subpopulation over 20,000 binaries that do not. As expected, the population of chirping binaries is heavily skewed toward high frequency, high chirp mass systems, with little or no preference for nearby systems. The population of non-chirping binaries is still biased toward frequencies above about 1 mHz. There is an overabundance of higher mass systems than is present in the complete Galactic population.

  6. Properties of planets in binary systems. The role of binary separation

    E-Print Network [OSTI]

    S. Desidera; M. Barbieri

    2006-10-20T23:59:59.000Z

    The statistical properties of planets in binaries were investigated. Any difference to planets orbiting single stars can shed light on the formation and evolution of planetary systems. As planets were found around components of binaries with very different separation and mass ratio, it is particularly important to study the characteristics of planets as a function of the effective gravitational influence of the companion. A compilation of planets in binary systems was made; a search for companions orbiting stars recently shown to host planets was performed, resulting in the addition of two further binary planet hosts (HD 20782 and HD 109749). The probable original properties of the three binary planet hosts with white dwarfs companions were also investigated. Using this updated sample of planets in binaries we performed a statistical analysis of the distributions of planet mass, period, and eccentricity, fraction of multiplanet systems, and stellar metallicity for planets orbiting components of tight and wide binaries and single stars. The only highly significant difference revealed by our analysis concerns the mass distribution of short-period planets. Massive planets in short period orbits are found in most cases around the components of rather tight binaries. The properties of exoplanets orbiting the components of wide binaries are compatible with those of planets orbiting single stars, except for a possible greater abundance of high-eccentricity planets. The previously suggested lack of massive planets with P>100 days in binaries is not confirmed. We conclude that the presence of a stellar companion with separation smaller than 100-300 AU is able to modify the formation and/or migration and/or the dynamical evolution history of giant planets while wide companions play a more limited role

  7. Detached white-dwarf close-binary stars -- CV's extended family

    E-Print Network [OSTI]

    T. R. Marsh

    1999-06-07T23:59:59.000Z

    I review detached binaries consisting of white dwarfs with either other white dwarfs or low mass main-sequence stars in tight orbits around them. Orbital periods have been measured for 15 white dwarf/white dwarf systems and 22 white dwarf/M dwarf systems. While small compared to the number of periods known for CVs (>300), I argue that each variety of detached system has a space density an order of magnitude higher that of CVs. While theory matches the observed distribution of orbital periods of the white dwarf/white dwarf binaries, it predicts white dwarfs of much lower mass than observed. Amongst both types of binary are clear examples of helium core white dwarfs, as opposed to the usual CO composition; similar systems must exist amongst the CVs. White dwarf/M dwarf binaries suffer from selection effects which diminish the numbers seen at long and short periods. They are useful for the study of irradiation; I discuss evidence to suggest that Balmer emission is broadened by optical depth effects to an extent which limits its usefulness for imaging the secondary stars in CVs.

  8. The Binary White Dwarf LHS 3236

    E-Print Network [OSTI]

    Harris, Hugh; Dupuy, Trent; Canzian, Blaise; Guetter, Harry; Hartkopf, William; Ireland, Michael; Leggett, Sandy; Levine, Stephen; Liu, Michael; Luginbuhl, Christian; Monet, Alice; Stone, Ronald; Subasavage, John; Tilleman, Trudy; Walker, Richard

    2013-01-01T23:59:59.000Z

    The white dwarf LHS 3236 (WD1639+153) is shown to be a double-degenerate binary, with each component having a high mass. Astrometry at the U.S. Naval Observatory gives a parallax and distance of 30.86 +/- 0.25 pc and a tangential velocity of 98 km/s, and reveals binary orbital motion. The orbital parameters are determined from astrometry of the photocenter over more than three orbits of the 4.0-year period. High-resolution imaging at the Keck Observatory resolves the pair with a separation of 31 and 124 mas at two epochs. Optical and near-IR photometry give a set of possible binary components. Consistency of all data indicates that the binary is a pair of DA stars with temperatures near 8000 and 7400 K and with masses of 0.93 and 0.91 M_solar; also possible, is a DA primary and a helium DC secondary with temperatures near 8800 and 6000 K and with masses of 0.98 and 0.69 M_solar. In either case, the cooling ages of the stars are ~3 Gyr and the total ages are <4 Gyr. The combined mass of the binary (1.66--1....

  9. The binary white dwarf LHS 3236

    SciTech Connect (OSTI)

    Harris, Hugh C.; Dahn, Conard C.; Canzian, Blaise; Guetter, Harry H.; Levine, Stephen E.; Luginbuhl, Christian B.; Monet, Alice K. B.; Stone, Ronald C.; Subasavage, John P.; Tilleman, Trudy; Walker, Richard L. [US Naval Observatory, 10391 West Naval Observatory Road, Flagstaff, AZ 86001-8521 (United States); Dupuy, Trent J.; Liu, Michael C. [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States); Hartkopf, William I. [US Naval Observatory, 3450 Massachusetts Avenue, N.W., Washington, DC 20392-5420 (United States); Ireland, Michael J. [Department of Physics and Astronomy, Macquarie University, New South Wales, NSW 2109 (Australia); Leggett, S. K., E-mail: hch@nofs.navy.mil [Gemini Observatory, 670 N. Aohoku Place, Hilo, HI 96720 (United States)

    2013-12-10T23:59:59.000Z

    The white dwarf LHS 3236 (WD1639+153) is shown to be a double-degenerate binary, with each component having a high mass. Astrometry at the U.S. Naval Observatory gives a parallax and distance of 30.86 ± 0.25 pc and a tangential velocity of 98 km s{sup –1}, and reveals binary orbital motion. The orbital parameters are determined from astrometry of the photocenter over more than three orbits of the 4.0 yr period. High-resolution imaging at the Keck Observatory resolves the pair with a separation of 31 and 124 mas at two epochs. Optical and near-IR photometry give a set of possible binary components. Consistency of all data indicates that the binary is a pair of DA stars with temperatures near 8000 and 7400 K and with masses of 0.93 and 0.91 M {sub ?}; also possible is a DA primary and a helium DC secondary with temperatures near 8800 and 6000 K and with masses of 0.98 and 0.69 M {sub ?}. In either case, the cooling ages of the stars are ?3 Gyr and the total ages are <4 Gyr. The combined mass of the binary (1.66-1.84 M {sub ?}) is well above the Chandrasekhar limit; however, the timescale for coalescence is long.

  10. Investigating Dark Energy with Black Hole Binaries

    E-Print Network [OSTI]

    Laura Mersini-Houghton; Adam Kelleher

    2009-06-08T23:59:59.000Z

    The accelerated expansion of the universe is ascribed to the existence of dark energy. Black holes accretion of dark energy induces a mass change proportional to the energy density and pressure of the background dark energy fluid. The time scale during which the mass of black holes changes considerably is too long relative to the age of the universe, thus beyond detection possibilities. We propose to take advantage of the modified black hole masses for exploring the equation of state $w[z]$ of dark energy, by investigating the evolution of supermassive black hole binaries on a dark energy background. Deriving the signatures of dark energy accretion on the evolution of binaries, we find that dark energy imprints on the emitted gravitational radiation and on the changes in the orbital radius of the binary can be within detection limits for certain supermassive black hole binaries. In this talk I describe how binaries can provide a useful tool in obtaining complementary information on the nature of dark energy, based on the work done with A.Kelleher.

  11. 3D Duo Binary Turbo Decoder Hardware Implementation

    E-Print Network [OSTI]

    Timo Lehngik-emden; Matthias Alles; Norbert Wehn

    Abstract: Each digital communication system needs channel coding to provide a certain quality of service. With the introducation of advanced channel codes like turbo codes and LDPC codes, error correcting near theoretical shannon limit became possible. Many applications require a low error floor in addition. The classical turbo code cannot meet this demand. Increasing the number of components codes, non-binary component codes or code concatenation are solutions for this problem, but come with a large complexity increase. In 2007 a new class of turbo codes, the 3D turbo code, was introduced by Berrou. The 3D turbo code provides a very good convergence and a large minimum distance at a low complexity. To the best of our knowledge this paper presents the first hardware implementation of a 3D turbo decoder. In addition we compare the implementation complexity of the 3D turbo decoder with the 8 and 16-state duo binary turbo decoder on FPGA and in 65nm ASIC technology.

  12. Tracking Multiple Targets Using Binary Decisions from Wireless Sensor Networks

    E-Print Network [OSTI]

    Michailidis, George

    Tracking Multiple Targets Using Binary Decisions from Wireless Sensor Networks Natallia Katenka- tions. 1 #12;Keywords: wireless sensor networks, binary data, target tracking, multiple targets, penal- ized maximum likelihood 1 Introduction and Problem Motivation Wireless Sensor Networks (WSN) have

  13. Binary Capture Rates for Massive Protostars

    E-Print Network [OSTI]

    Nickolas Moeckel; John Bally

    2007-04-09T23:59:59.000Z

    The high multiplicity of massive stars in dense, young clusters is established early in their evolution. The mechanism behind this remains unresolved. Recent results suggest that massive protostars may capture companions through disk interactions with much higher efficiency than their solar mass counterparts. However, this conclusion is based on analytic determinations of capture rates and estimates of the robustness of the resulting binaries. We present the results of coupled n-body and SPH simulations of star-disk encounters to further test the idea that disk-captured binaries contribute to the observed multiplicity of massive stars.

  14. Binary Evolution in World Wide Web

    E-Print Network [OSTI]

    S. N. Nazin; V. M. Lipunov; I. E. Panchenko; K. A. Postnov; M. E. Prokhorov; S. B. Popov

    1996-05-29T23:59:59.000Z

    We present a WWW-version of the {\\it Scenario Machine} - a computer code designed to calculate the evolution of close binary stellar systems. The Internet users can directly access to the code and calculate binary evolutionary tracks with parameters at the user's will. The program is running on the {\\it Pentium} server of the Division of the Relativistic Astrophysics of the Sternberg Astronimical Institute (http://xray.sai.msu.su/ ). The results are presented both in the form of tables and graphic diagrams. The work is always in progress. More possibilities for Internet users are intended to become available in the near future.

  15. RESEARCH Open Access Multi-non-binary turbo codes

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    RESEARCH Open Access Multi-non-binary turbo codes Horia Balta1,2 , Catherine Douillard3 and Radu Lucaciu1* Abstract This paper presents a new family of turbo codes called multi-non-binary turbo codes (MNBTCs) that generalizes the concept of turbo codes to multi-non-binary (MNB) parallel concatenated

  16. Resurvey of order and chaos in spinning compact binaries

    SciTech Connect (OSTI)

    Wu Xin [Department of Physics, Nanchang University, Nanchang 330031 (China); Xie Yi [Department of Astronomy, Nanjing University, Nanjing 210093 (China)

    2008-05-15T23:59:59.000Z

    This paper is mainly devoted to applying the invariant, fast, Lyapunov indicator to clarify some doubt regarding the apparently conflicting results of chaos in spinning compact binaries at the second-order post-Newtonian approximation of general relativity from previous literatures. It is shown with a number of examples that no single physical parameter or initial condition can be described as responsible for causing chaos, but a complicated combination of all parameters and initial conditions is responsible. In other words, a universal rule for the dependence of chaos on each parameter or initial condition cannot be found in general. Chaos does not depend only on the mass ratio, and the maximal spins do not necessarily bring the strongest effect of chaos. Additionally, chaos does not always become drastic when the initial spin vectors are nearly perpendicular to the orbital plane, and the alignment of spins cannot trigger chaos by itself.

  17. Hydrogen deficient donors in low-mass X-ray binaries

    E-Print Network [OSTI]

    Gijs Nelemans

    2007-11-05T23:59:59.000Z

    A number of X-ray binaries (neutron stars or black holes accreting from a companion star) have such short orbital periods that ordinary, hydrogen rich, stars do not fit in. Instead the mass-losing star must be a compact, evolved star, leading to the transfer of hydrogen deficient material to the neutron star. I discuss the current knowledge of these objects, with focus on optical spectroscopy.

  18. The Formation of Population III Binaries

    E-Print Network [OSTI]

    Kazuya Saigo; Tomoaki Matsumoto; Masayuki Umemura

    2004-10-29T23:59:59.000Z

    We explore the possibility for the formation of Population III binaries. The collapse of a rotating cylinder is simulated with a three-dimensional, high-resolution nested grid, assuming the thermal history of primordial gas. The simulations are done with dimensionless units, and the results are applicable to low-mass as well as massive systems by scaling with the initial density. We find that if the initial angular momentum is as small as $\\beta \\approx 0.1$, where $\\beta$ is the ratio of centrifugal force to pressure force, then the runaway collapse of the cloud stops to form a rotationally-supported disk. After the accretion of the envelope, the disk undergoes a ring instability, eventually fragmenting into a binary. If the initial angular momentum is relatively large, a bar-type instability arises, resulting in the collapse into a single star through rapid angular momentum transfer. The present results show that a significant fraction of Pop III stars are expected to form in binary systems, even if they are quite massive or less massive. The cosmological implications of Population III binaries are briefly discussed.

  19. Jitter Equalization for Binary Baseband Communication

    E-Print Network [OSTI]

    Chan Carusone, Tony

    Jitter Equalization for Binary Baseband Communication Anthony Chan Carusone Department reduces pattern- dependent jitter. Instead of using the LMS or a related algorithm that optimizes at data transitions, thereby targeting zero jitter. The LMS algorithm is modified to combine the two

  20. Binary translation using peephole translation rules

    DOE Patents [OSTI]

    Bansal, Sorav; Aiken, Alex

    2010-05-04T23:59:59.000Z

    An efficient binary translator uses peephole translation rules to directly translate executable code from one instruction set to another. In a preferred embodiment, the translation rules are generated using superoptimization techniques that enable the translator to automatically learn translation rules for translating code from the source to target instruction set architecture.

  1. Principal Components Analysis for Binary Data

    E-Print Network [OSTI]

    Lee, Seokho

    2010-07-14T23:59:59.000Z

    . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . ix CHAPTER I INTRODUCTION . . . . . . . . . . . . . . . . . . . . . . . . . . 1 1.1 Formulations of Principal Components Analysis . . . . . . . . 2 1.2 Generalization of Sparse Principal Components Analysis to Binary Variables... . . . . . . . . . . . . . . . . . . . . . . . . 8 1.3 Review of Estimation Procedures . . . . . . . . . . . . . . . . 11 1.4 Overview of Dissertation . . . . . . . . . . . . . . . . . . . . . 18 II SPARSE PRINCIPAL COMPONENTS ANALYSIS FOR BI- NARY DATA...

  2. Non-binary Entanglement-assisted Stabilizer Quantum Codes

    E-Print Network [OSTI]

    Leng Riguang; Ma Zhi

    2011-05-30T23:59:59.000Z

    In this paper, we show how to construct non-binary entanglement-assisted stabilizer quantum codes by using pre-shared entanglement between the sender and receiver. We also give an algorithm to determine the circuit for non-binary entanglement-assisted stabilizer quantum codes and some illustrated examples. The codes we constructed do not require the dual-containing constraint, and many non-binary classical codes, like non-binary LDPC codes, which do not satisfy the condition, can be used to construct non-binary entanglement-assisted stabilizer quantum codes.

  3. Probability distribution function for inclinations of merging compact binaries detected by gravitational wave interferometers

    E-Print Network [OSTI]

    Naoki Seto

    2014-10-20T23:59:59.000Z

    We analytically discuss probability distribution function (PDF) for inclinations of merging compact binaries whose gravitational waves are coherently detected by a network of ground based interferometers. The PDF would be useful for studying prospects of (1) simultaneously detecting electromagnetic signals (such as gamma-ray-bursts) associated with binary mergers and (2) statistically constraining the related theoretical models from the actual observational data of multi-messenger astronomy. Our approach is similar to Schutz (2011), but we explicitly include the dependence of the polarization angles of the binaries, based on the concise formulation given in Cutler and Flanagan (1994). We find that the overall profiles of the PDFs are similar for any networks composed by the second generation detectors (Advanced-LIGO, Advanced-Virgo, KAGRA, LIGO-India). For example, 5.1% of detected binaries would have inclination angle less than 10 degree with at most 0.1% differences between the potential networks. A perturbative expression is also provided for generating the PDFs with a small number of parameters given by directional averages of the quantity $\\epsilon$ that characterises the asymmetry of network sensitivities to incoming two orthogonal polarization modes.

  4. Filtering post-Newtonian gravitational waves from coalescing binaries

    E-Print Network [OSTI]

    B. S. Sathyaprakash

    1994-11-15T23:59:59.000Z

    Gravitational waves from inspiralling binaries are expected to be detected using a data analysis technique known as {\\it matched filtering.} This technique is applicable whenever the form of the signal is known accurately. Though we know the form of the signal precisely, we will not know {\\it a priori} its parameters. Hence it is essential to filter the raw output through a host of search templates each corresponding to different values of the parameters. The number of search templates needed in detecting the Newtonian waveform characterized by three independent parameters is itself several thousands. With the inclusion of post-Newtonian corrections the inspiral waveform will have four independent parameters and this, it was thought, would lead to an increase in the number of filters by several orders of magnitude---an unfavorable feature since it would drastically slow down data analysis. In this paper I show that by a judicious choice of signal parameters we can work, even when the first post-Newtonian corrections are included, with as many number of parameters as in the Newtonian case. In other words I demonstrate that the effective dimensionality of the signal parameter space does not change when first post-Newtonian corrections are taken into account.

  5. Evolution of Close Neutron Star Binaries

    E-Print Network [OSTI]

    W. Ogawaguchi; Y. Kojima

    1996-10-17T23:59:59.000Z

    We have calculated evolution of neutron star binaries towards the coalescence driven by gravitational radiation. The hydrodynamical effects as well as the general relativistic effects are important in the final phase. All corrections up to post$^{2.5}$-Newtonian order and the tidal effect are included in the orbital motion. The star is approximated by a simple Newtonian stellar model called affine star model. Stellar spins and angular momentum are assumed to be aligned. We have showed how the internal stellar structure affects the stellar deformation, variations of the spins, and the orbital motion of the binary just before the contact. The gravitational wave forms from the last a few revolutions significantly depend on the stellar structure.

  6. American Institute of Aeronautics and Astronautics Practical Software Engineering Strategies for Scientific

    E-Print Network [OSTI]

    Roy, Chris

    , nuclear power plants, and medical devices (e.g., pacemakers). Software engineering is an enormously broad tolerance used, the number of significant figures used in the floating point computations, etc. The goal

  7. Evolution of Compact-Binary Populations in Globular Clusters: A Boltzmann Study II. Introducing Stochasticity

    E-Print Network [OSTI]

    Sambaran Banerjee; Pranab Ghosh

    2008-04-14T23:59:59.000Z

    We continue exploration of the Boltzmann scheme started in Banerjee and Ghosh (2007, henceforth Paper I) for studying the evolution of compact-binary populations of globular clusters, introducing in this paper our method of handling the stochasticity inherent in dynamical processes of binary formation, destruction and hardening in globular clusters. We describe these stochastic processes as "Wiener processes", whereupon the Boltzmann equation becomes a stochastic partial differential equation, the solution of which requires the use of "Ito calculus" (this use being the first, to our knowledge, in this subject), in addition to ordinary calculus. We focus on the evolution of (a) the number of X-ray binaries $N_{XB}$ in globular clusters, and (b) the orbital-period distribution of these binaries. We show that, although the details of the fluctuations in the above quantities differ from one "realization" to another of the stochastic processes, the general trends follow those found in the continuous-limit study of Paper I, and the average result over many such realizations is close to the continuous-limit result. We investigate the dependence of $N_{XB}$ found by these calculations on two essential globular-cluster parameters, namely, the star-star and star-binary encounter-rate parameters $\\Gamma$ and $\\gamma$, for which we had coined the name Verbunt parameters in Paper I. We compare our computed results with those from CHANDRA observations of Galactic globular clusters, showing that the expected scalings of $N_{XB}$ with the Verbunt parameters are in good agreement with the observed ones. We indicate what additional features can be incorporated into the scheme in future, and how more elaborate problems can be tackled.

  8. Long-Term Stability of Planets in Binary Systems

    E-Print Network [OSTI]

    Matthew Holman; Paul Wiegert

    1998-09-24T23:59:59.000Z

    A simple question of celestial mechanics is investigated: in what regions of phase space near a binary system can planets persist for long times? The planets are taken to be test particles moving in the field of an eccentric binary system. A range of values of the binary eccentricity and mass ratio is studied, and both the case of planets orbiting close to one of the stars, and that of planets outside the binary orbiting the system's center of mass, are examined. From the results, empirical expressions are developed for both 1) the largest orbit around each of the stars, and 2) the smallest orbit around the binary system as a whole, in which test particles survive the length of the integration (10^4 binary periods). The empirical expressions developed, which are roughly linear in both the mass ratio mu and the binary eccentricity e, are determined for the range 0.0 <= e <= 0.7-0.8 and 0.1 <= mu <= 0.9 in both regions, and can be used to guide searches for planets in binary systems. After considering the case of a single low-mass planet in binary systems, the stability of a mutually-interacting system of planets orbiting one star of a binary system is examined, though in less detail.

  9. On the Neutron Star-Black Hole Binaries Produced by Binary-driven Hypernovae

    E-Print Network [OSTI]

    Fryer, C L; Rueda, J A; Ruffini, R

    2015-01-01T23:59:59.000Z

    Binary-driven hypernovae (BdHNe) following the induced gravitational collapse (IGC) paradigm have been introduced to explain the concomitance of energetic long gamma-ray bursts (GRBs) with type Ic supernovae. The progenitor system is a tight binary system composed of a carbon-oxygen (CO) core and a neutron star (NS) companion. The supernova ejecta of the exploding CO core triggers a hypercritical accretion process onto the NS, which in a few seconds reach the NS critical mass, and gravitationally collapses to a black hole (BH) emitting a GRB. These tight binary systems evolve through the supernova explosion very differently than compact binary progenitors studied in population synthesis calculations. First, the hypercritical accretion onto the NS companion alters both the mass and momentum of the binary. Second, because the explosion timescale is on par with the orbital period, the mass ejection can not be assumed to be instantaneous. Finally, the bow shock created as the accreting NS plows through the supern...

  10. Automated pupil remapping with binary optics

    DOE Patents [OSTI]

    Neal, Daniel R. (Tijeras, NM); Mansell, Justin (Albuquerque, NM)

    1999-01-01T23:59:59.000Z

    Methods and apparatuses for pupil remapping employing non-standard lenslet shapes in arrays; divergence of lenslet focal spots from on-axis arrangements; use of lenslet arrays to resize two-dimensional inputs to the array; and use of lenslet arrays to map an aperture shape to a different detector shape. Applications include wavefront sensing, astronomical applications, optical interconnects, keylocks, and other binary optics and diffractive optics applications.

  11. Automated pupil remapping with binary optics

    DOE Patents [OSTI]

    Neal, D.R.; Mansell, J.

    1999-01-26T23:59:59.000Z

    Methods and apparatuses are disclosed for pupil remapping employing non-standard lenslet shapes in arrays; divergence of lenslet focal spots from on-axis arrangements; use of lenslet arrays to resize two-dimensional inputs to the array; and use of lenslet arrays to map an aperture shape to a different detector shape. Applications include wavefront sensing, astronomical applications, optical interconnects, keylocks, and other binary optics and diffractive optics applications. 24 figs.

  12. Hyper Space Complex Number

    E-Print Network [OSTI]

    Shanguang Tan

    2007-04-23T23:59:59.000Z

    A new kind of numbers called Hyper Space Complex Numbers and its algebras are defined and proved. It is with good properties as the classic Complex Numbers, such as expressed in coordinates, triangular and exponent forms and following the associative and commutative laws of addition and multiplication. So the classic Complex Number is developed from in complex plane with two dimensions to in complex space with N dimensions and the number system is enlarged also.

  13. The Formation of Population III Binaries

    E-Print Network [OSTI]

    Saigo, K; Umemura, M; Saigo, Kazuya; Matsumoto, Tomoaki; Umemura, Masayuki

    2004-01-01T23:59:59.000Z

    We explore the possibility for the formation of Population III binaries. The collapse of a rotating cylinder is simulated with a three-dimensional, high-resolution nested grid, assuming the thermal history of primordial gas. The simulations are done with dimensionless units, and the results are applicable to low-mass as well as massive systems by scaling with the initial density. We find that if the initial angular momentum is as small as $\\beta \\approx 0.1$, where $\\beta$ is the ratio of centrifugal force to pressure force, then the runaway collapse of the cloud stops to form a rotationally-supported disk. After the accretion of the envelope, the disk undergoes a ring instability, eventually fragmenting into a binary. If the initial angular momentum is relatively large, a bar-type instability arises, resulting in the collapse into a single star through rapid angular momentum transfer. The present results show that a significant fraction of Pop III stars are expected to form in binary systems, even if they ar...

  14. Gravitational lensing in eclipsing binary stars

    E-Print Network [OSTI]

    T. R. Marsh

    2000-12-18T23:59:59.000Z

    I consider the effect of the gravitational deflection of light upon the light curves of eclipsing binary stars, focussing mainly upon systems containing at least one white dwarf component. In absolute terms the effects are small, however they are strongest at the time of secondary eclipse when the white dwarf transits its companion, and act to reduce the depth of this feature. If not accounted for, this may lead to under-estimation of the radius of the white dwarf compared to that of its companion. I show that the effect is significant for plausible binary parameters, and that it leads to ~25% reduction in the transit depth in the system KPD 1930+2752. The reduction of eclipse depth is degenerate with the stellar radius ratio, and therefore cannot be used to establish the existence of lensing. A second order effect of the light bending is to steepen the ingress and egress features of the secondary eclipse relative to the primary eclipse, although it will be difficult to see this in practice. I consider also binaries containing neutron stars and black-holes. I conclude that, although relatively large effects are possible in such systems, a combination of rarity, faintness and intrinsic variability make it unlikely that lensing will be detectable in them.

  15. Phase equilibrium measurements on twelve binary mixtures

    SciTech Connect (OSTI)

    Giles, N.F. [Wiltec Research Co., Inc., Provo, UT (United States)] [Wiltec Research Co., Inc., Provo, UT (United States); Wilson, H.L.; Wilding, W.V. [Brigham Young Univ., Provo, UT (United States). Chemical Engineering Dept.] [Brigham Young Univ., Provo, UT (United States). Chemical Engineering Dept.

    1996-11-01T23:59:59.000Z

    Phase equilibrium measurements have been performed on twelve binary mixtures. The PTx method was used to obtain vapor-liquid equilibrium data for the following binary systems at two temperatures each: ethanethiol + propylene; nitrobenzene + methanol; pyridine + ethyl acetate; octane + tert-amyl methyl ether; diisopropyl ether + butane; 1,3-dichloro-2-propanol + epichlorohydrin; 2,3-dichloro-1-propanol + epichlorohydrin; 2,3-epoxy-1-propanol + epichlorohydrin; 3-chloro-1,2-propanediol + epichlorohydrin; methanol + hydrogen cyanide. For these systems, equilibrium vapor and liquid phase compositions were derived from the PTx data using the Soave equation of state to represent the vapor phase and the Wilson, NRTL, or Redlich-Kister activity coefficient model to represent the liquid phase. The infinite dilution activity coefficient of methylamine in N-methyl-2-pyrrolidone was determined at three temperatures by performing PTx measurements on the N-methyl-2-pyrrolidone was determined at three temperatures by performing PTx measurements on the N-methyl-2-pyrrolidone-rich half of the binary. Liquid-liquid equilibrium studies were made on the triethylene glycol + 1-pentene system at two temperatures by directly analyzing samples taken from each liquid phase.

  16. Measuring the configurational temperature of a binary disc packing

    E-Print Network [OSTI]

    Song-Chuan Zhao; Matthias Schröter

    2014-06-20T23:59:59.000Z

    Jammed packings of granular materials differ from systems normally described by statistical mechanics in that they are athermal. In recent years a statistical mechanics of static granular media has emerged where the thermodynamic temperature is replaced by a configurational temperature X which describes how the number of mechanically stable configurations depends on the volume. Four different methods have been suggested to measure X. Three of them are computed from properties of the Voronoi volume distribution, the fourth takes into account the contact number and the global volume fraction. This paper answers two questions using experimental binary disc packings: First we test if the four methods to measure compactivity provide identical results when applied to the same dataset. We find that only two of the methods agree quantitatively. Secondly, we test if X is indeed an intensive variable; this becomes true only for samples larger than roughly 200 particles. This result is shown to be due to recently found correlations between the particle volumes [Zhao et al., Europhys. Lett., 2012, 97, 34004].

  17. Angular momentum exchange in white dwarf binaries accreting through direct impact

    SciTech Connect (OSTI)

    Sepinsky, J. F. [Department of Physics and Electrical Engineering, The University of Scranton, Scranton, PA 18510 (United States); Kalogera, V., E-mail: jeremy.sepinsky@scranton.edu, E-mail: vicky@northwestern.edu [Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208 (United States)

    2014-04-20T23:59:59.000Z

    We examine the exchange of angular momentum between the component spins and the orbit in semi-detached double white dwarf binaries undergoing mass transfer through direct impact of the transfer stream. We approximate the stream as a series of discrete massive particles ejected in the ballistic limit at the inner Lagrangian point of the donor toward the accretor. This work improves upon similar earlier studies in a number of ways. First, we self-consistently calculate the total angular momentum of the orbit at all times. This includes changes in the orbital angular momentum during the ballistic trajectory of the ejected mass, as well as changes during the ejection/accretion due to the radial component of the particle's velocity. Second, we calculate the particle's ballistic trajectory for each system, which allows us to determine the precise position and velocity of the particle upon accretion. We can then include specific information about the radius of the accretor as well as the angle of impact. Finally, we ensure that the total angular momentum is conserved, which requires the donor star spin to vary self-consistently. With these improvements, we calculate the angular momentum change of the orbit and each binary component across the entire parameter space of direct impact double white dwarf binary systems. We find a significant decrease in the amount of angular momentum removed from the orbit during mass transfer, as well as cases where this process increases the angular momentum of the orbit at the expense of the spin angular momentum of the donor. We conclude that, unlike earlier claims in the literature, mass transfer through direct impact need not destabilize the binary and that the quantity and sign of the orbital angular momentum transfer depends on the binary properties, particularly the masses of the double white dwarf binary component stars. This stabilization may significantly impact the population synthesis calculations of the expected numbers of events/systems for which double white dwarfs may be a progenitor, e.g., Type Ia supernovae, Type.Ia supernovae, and AM CVn.

  18. BINARY CEPHEIDS: SEPARATIONS AND MASS RATIOS IN 5 M {sub ?} BINARIES

    SciTech Connect (OSTI)

    Evans, Nancy Remage; Karovska, Margarita; Tingle, Evan [Smithsonian Astrophysical Observatory, MS 4, 60 Garden Street, Cambridge, MA 02138 (United States); Bond, Howard E. [Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States); Schaefer, Gail H. [The CHARA Array, Georgia State University, P.O. Box 3965, Atlanta, GA 30302-3965 (United States); Mason, Brian D., E-mail: nevans@cfa.harvard.edu, E-mail: heb11@psu.edu, E-mail: schaefer@chara-array.org [US Naval Observatory, 3450 Massachusetts Avenue, NW, Washington, DC 20392-5420 (United States)

    2013-10-01T23:59:59.000Z

    Deriving the distribution of binary parameters for a particular class of stars over the full range of orbital separations usually requires the combination of results from many different observing techniques (radial velocities, interferometry, astrometry, photometry, direct imaging), each with selection biases. However, Cepheids—cool, evolved stars of ?5 M {sub ?}—are a special case because ultraviolet (UV) spectra will immediately reveal any companion star hotter than early type A, regardless of the orbital separation. We have used International Ultraviolet Explorer UV spectra of a complete sample of all 76 Cepheids brighter than V = 8 to create a list of all 18 Cepheids with companions more massive than 2.0 M {sub ?}. Orbital periods of many of these binaries are available from radial-velocity studies, or can be estimated for longer-period systems from detected velocity variability. In an imaging survey with the Hubble Space Telescope Wide Field Camera 3, we resolved three of the companions (those of ? Aql, S Nor, and V659 Cen), allowing us to make estimates of the periods out to the long-period end of the distribution. Combining these separations with orbital data in the literature, we derive an unbiased distribution of binary separations, orbital periods, and mass ratios. The distribution of orbital periods shows that the 5 M {sub ?} binaries have systematically shorter periods than do 1 M {sub ?} stars. Our data also suggest that the distribution of mass ratios depends on both binary separation and system multiplicity. The distribution of mass ratios as a function of orbital separation, however, does not depend on whether a system is a binary or a triple.

  19. Targeting the optimal design in randomized clinical trials with binary outcomes and no covariate

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    Targeting the optimal design in randomized clinical trials with binary outcomes and no covariate of randomized clinical trials with binary treatment, binary outcome and no covariate. By adaptive design, we designs in the case of randomized clinical trials with binary treatment, binary outcome and no covariate

  20. Collisional Hardening of Compact Binaries in Globular Clusters

    E-Print Network [OSTI]

    S. Banerjee; P. Ghosh

    2006-09-29T23:59:59.000Z

    We consider essential mechanisms for orbit-shrinkage or "hardening" of compact binaries in globular clusters to the point of Roche-lobe contact and X-ray emission phase, focussing on the process of collisional hardening due to encounters between binaries and single stars in the cluster core. The interplay between this kind of hardening and that due to emission of gravitational radiation produces a characteristic scaling of the orbit-shrinkage time with the single-star binary encounter rate $\\gamma$ in the cluster which we introduce, clarify, and explore. We investigate possible effects of this scaling on populations of X-ray binaries in globular clusters within the framework of a simple "toy" scheme for describing the evolution of pre-X-ray binaries in globular clusters. We find the expected qualitative trends sufficiently supported by data on X-ray binaries in galactic globular clusters to encourage us toward a more quantitative study.

  1. The Relativistic Binary Pulsar B1913+16

    E-Print Network [OSTI]

    J. M. Weisberg; J. H. Taylor

    2002-11-11T23:59:59.000Z

    We describe the results of a relativistic analysis of our observations of binary pulsar B1913+16, up to the latest measurements in 2001 August.

  2. Binary Decision Rules for Multistage Adaptive Mixed-Integer ...

    E-Print Network [OSTI]

    2014-08-20T23:59:59.000Z

    Aug 20, 2014 ... In the first test series, we compared the performance of the binary decision rules versus the non- ..... involving indicator functions is NP-hard.

  3. Binary Cycle Power Plant | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page onYou are now leaving Energy.gov You are now leaving Energy.gov You are being directedAnnualProperty EditCalifornia: EnergyAvignon,Belcher Homes JumpMaintenance |BigBig WindyWindBinary

  4. Dispersal of planets hosted in binaries, transitional members of multiple star systems

    E-Print Network [OSTI]

    F. Marzari; M. Barbieri

    2007-07-04T23:59:59.000Z

    This paper explains why planets in binary star systems might have a lower frequency. A transient triple state of the binary causes the dispersal of planets.

  5. Disk Evolution in Young Binaries: from Observations to Theory

    E-Print Network [OSTI]

    J. -L. Monin; C. J. Clarke; L. Prato; C. McCabe

    2006-04-03T23:59:59.000Z

    The formation of a binary system surrounded by disks is the most common outcome of stellar formation. Hence studying and understanding the formation and the evolution of binary systems and associated disks is a cornerstone of star formation science. Moreover, since the components within binary systems are coeval and the sizes of their disks are fixed by the tidal truncation of their companion, binary systems provide an ideal "laboratory" in which to study disk evolution under well defined boundary conditions. In this paper, we review observations of several inner disk diagnostics in multiple systems, including hydrogen emission lines (indicative of ongoing accretion), $K-L$ and $K-N$ color excesses (evidence of warm inner disks), and polarization (indicative of the relative orientations of the disks around each component). We examine to what degree these properties are correlated within binary systems and how this degree of correlation depends on parameters such as separation and binary mass ratio. These findings will be interpreted both in terms of models that treat each disk as an isolated reservoir and those in which the disks are subject to re-supply from some form of circumbinary reservoir, the observational evidence for which we will also critically review. The planet forming potential of multiple star systems is discussed in terms of the relative lifetimes of disks around single stars, binary primaries and binary secondaries. Finally, we summarize several potentially revealing observational problems and future projects that could provide further insight into disk evolution in the coming decade

  6. Layered Binary-Dielectrics for Energy Applications: Limitations and Potentials

    SciTech Connect (OSTI)

    Tuncer, Enis [ORNL

    2012-01-01T23:59:59.000Z

    In this Letter, an attempt is made to illustrate how performance of an electrically insulating material, a dielectric, can be improved by constructing a layered binary-dielectric structure that employs a weak insulator with high dielectric permittivity. It is shown that layered binary-dielectrics could have a signicant impact on energy storage and electrical insulation.

  7. Binary coding of Kekule structures of catacondensed benzenoid hydrocarbons

    E-Print Network [OSTI]

    Klavzar, Sandi

    Binary coding of Kekul´e structures of catacondensed benzenoid hydrocarbons Sandi Klavzar of benzenoids Key words: benzenoid hydrocarbons, benzenoid graph, resonance graph, Kekul´e structure, algorithm easily be recovered from its binary code. Key words: benzenoid hydrocarbons, benzenoid graph, resonance

  8. Binary coding of Kekule structures of catacondensed benzenoid hydrocarbons

    E-Print Network [OSTI]

    Klavzar, Sandi

    Binary coding of Kekulâ??e structures of catacondensed benzenoid hydrocarbons Sandi KlavŸzar, aâ??e structures of benzenoids Key words: benzenoid hydrocarbons, benzenoid graph, resonance graph, Kekul easily be recovered from its binary code. Key words: benzenoid hydrocarbons, benzenoid graph, resonance

  9. Optimum Treatment Allocation for Dualobjective Clinical Trials with Binary Outcomes

    E-Print Network [OSTI]

    New York at Stoney Brook, State University of

    Optimum Treatment Allocation for Dual­objective Clinical Trials with Binary Outcomes Wei Zhu, Weng treatment allocation schemes are derived for multiple­objective clinical trials with binary outcome­ tients to various treatment groups in a randomized controlled clinical trial where the primary outcome

  10. Contemporary Mathematics The merit factor of binary sequence families

    E-Print Network [OSTI]

    Jedwab, Jonathan

    Contemporary Mathematics The merit factor of binary sequence families constructed from m-sequences sequence families obtained from an initial binary sequence family using a "negaperiodic" and a "periodic" construction. When the initial sequences are m-sequences, both of the constructed families have the same

  11. Surface tension in a reactive binary mixture of incompressible fluids

    E-Print Network [OSTI]

    Struchtrup, Henning

    Surface tension in a reactive binary mixture of incompressible fluids Henning Struchtrup Institute with a distributed form of surface tension. The model describes chemistry, diffusion, viscosity and heat transfer tension at the front. Keywords: Binary mixtures, Surface tension, Irreversible thermodynamics, Hele

  12. ccsd00004127, ON THE SURFACE TENSIONS OF BINARY MIXTURES

    E-Print Network [OSTI]

    ccsd­00004127, version 1 ­ 2 Feb 2005 ON THE SURFACE TENSIONS OF BINARY MIXTURES JEAN RUIZ Abstract tensions and the concentrations are brie y reviewed. Key Words: Surface tensions, binary mixtures the corresponding surface tension depends on the composition of the mixture. Some relationship is expected which

  13. Hamiltonian Hydrodynamics and Irrotational Binary Inspiral

    E-Print Network [OSTI]

    Charalampos M. Markakis

    2014-10-28T23:59:59.000Z

    Gravitational waves from neutron-star and black-hole binaries carry valuable information on their physical properties and probe physics inaccessible to the laboratory. Although development of black-hole gravitational-wave templates in the past decade has been revolutionary, the corresponding work for double neutron-star systems has lagged. Neutron stars can be well-modelled as simple barotropic fluids during the part of binary inspiral most relevant to gravitational wave astronomy, but the crucial geometric and mathematical consequences of this simplification have remained computationally unexploited. In particular, Carter and Lichnerowicz have described barotropic fluid motion via classical variational principles as conformally geodesic. Moreover, Kelvin's circulation theorem implies that initially irrotational flows remain irrotational. Applied to numerical relativity, these concepts lead to novel Hamiltonian or Hamilton-Jacobi schemes for evolving relativistic fluid flows. Hamiltonian methods can conserve not only flux, but also circulation and symplecticity, and moreover do not require addition of an artificial atmosphere typically required by standard conservative methods. These properties can allow production of high-precision gravitational waveforms at low computational cost. This canonical hydrodynamics approach is applicable to a wide class of problems involving theoretical or computational fluid dynamics.

  14. Electrodeposition of binary iron-group alloys

    SciTech Connect (OSTI)

    Sasaki, K.Y.; Talbot, J.B. [Univ. of California, San Diego, La Jolla, CA (United States)

    1995-03-01T23:59:59.000Z

    Thin films of NiCo and CoFe have been galvanostatically electroplated onto a platinum rotating disk electrode from simple sulfate baths containing 0.5M of the more noble metal sulfate and 0.1M of the less noble metal sulfate. The experimental results are compared to those of previous studies of NiFe codeposition in order to study the anomalous codeposition behavior of the binary iron-group alloys. Comparison of the electrodeposition results indicates that codeposition of these binary alloys is not totally analogous. It was found that codeposition of NiCo and NiFe show more mass-transfer effects than does CoFe deposition within the range of current densities studied. A model of anomalous codeposition put forth previously for NiFe was applied to the electrodeposition of NiCo and CoFe to determine the extensibility of the model, which assumes metal mono hydroxides, MOH{sup +}, are the important charge-transfer species. This model was unable to characterize fully either NiCo or CoFe electrodeposition. However, with minor changes to the hydrolysis constants used in the model, the model predictions were found to agree with the data for CoFe codeposition and greatly, improve the fit for the NiCo results.

  15. Multispecies weighted Hurwitz numbers

    E-Print Network [OSTI]

    Harnad, J

    2015-01-01T23:59:59.000Z

    The construction of hypergeometric 2D Toda $\\tau$-functions as generating functions for weighted Hurwitz numbers is extended to multispecies families. Both the enumerative geometrical significance of multispecies weighted Hurwitz numbers as weighted enumerations of branched coverings of the Riemann sphere and their combinatorial significance in terms of weighted paths in the Cayley graph of $S_n$ are derived. The particular case of multispecies quantum weighted Hurwitz numbers is studied in detail.

  16. Curvature and Tachibana numbers

    SciTech Connect (OSTI)

    Stepanov, Sergey E [Finance Academy under the Government of the Russian Federation, Moscow (Russian Federation)

    2011-07-31T23:59:59.000Z

    The aim of this paper is to define the rth Tachibana number t{sub r} of an n-dimensional compact oriented Riemannian manifold as the dimension of the space of conformally Killing r-forms, for r=1,2,...,n-1. We also describe properties of these numbers, by analogy with properties of the Betti numbers b{sub r} of a compact oriented Riemannian manifold. Bibliography: 25 titles.

  17. SMA Observations of Class 0 Protostars: A High-Angular Resolution Survey of Protostellar Binary Systems

    E-Print Network [OSTI]

    Chen, Xuepeng; Zhang, Qizhou; Bourke, Tyler L; Launhardt, Ralf; Jorgensen, Jes K; Lee, Chin-Fee; Foster, Jonathan B; Dunham, Michael M; Pineda, Jaime E; Henning, Thomas

    2013-01-01T23:59:59.000Z

    We present high angular resolution 1.3 mm and 850 um dust continuum data obtained with the Submillimeter Array toward 33 Class 0 protostars in nearby clouds (distance < 500 pc), which represents so far the largest survey toward protostellar binary/multiple systems. The median angular resolution in the survey is 2.5 arcsec, while the median linear resolution is approximately 600 AU. Compact dust continuum emission is observed from all sources in the sample. Twenty-one sources in the sample show signatures of binarity/multiplicity, with separations ranging from 50 to 5000 AU. The numbers of singles, binaries, triples, and quadruples in the sample are 12, 14, 5, and 2, respectively. The derived multiplicity frequency (MF) and companion star fraction (CSF) for Class 0 protostars are 0.64+/-0.08 and 0.91+/-0.05, respectively, with no correction for completeness. The derived MF and CSF in this survey are approximately two times higher than the values found in the binary surveys toward Class I YSOs, and approxima...

  18. WR Populations in Starbursts: WN and WC Subtypes and the Role of Binaries

    E-Print Network [OSTI]

    Daniel Schaerer; William D. Vacca

    1996-09-28T23:59:59.000Z

    We present the first results of a new set of population synthesis models, which utilize the latest stellar evolutionary tracks, recent non-LTE atmosphere models which include stellar winds, and observed line strengths in WR spectra to predict the relative strengths of various WN and WC/WO emission features in the spectra of starburst galaxies. Our results will be used to derive accurate numbers of WN and WC stars in starburst galaxies. We also analyze the frequency and the WN and WC content of WR-rich galaxies in low metallicity samples; the theoretical predictions are found to be in good agreement with the observed frequencies. We also discuss the possible role of massive close binaries in starburst regions. If the starburst regions are formed in relatively instantaneous bursts we argue that, given their young age as derived from emission lines equivalent widths, (1) in the majority of the observed WR galaxies massive close binaries have not contributed significantly to the WR population, and (2) nebular HeII 4686 emission is very unlikely due to massive X-ray binaries.

  19. Multi-Color Coronagraph Experiment in a Vacuum Testbed with a Binary Shaped Pupil Mask

    E-Print Network [OSTI]

    Haze, Kanae; Abe, Lyu; Kotani, Takayuki; Nakagawa, Takao; Sato, Toshimichi; Yamamuro, Tomoyasu

    2011-01-01T23:59:59.000Z

    We conducted a number of multi-band coronagraph experiments using a vacuum chamber and a binary-shaped pupil mask which in principle should work at all wavelengths, in the context of the research and development on a coronagraph to observe extra-solar planets (exoplanets) directly. The aim of this work is to demonstrate that subtraction of Point Spread Function (PSF) and multi-band experiments using a binary-shaped pupil mask coronagraph would help improve the contrast in the observation of exoplanets. A checkerboard mask, a kind of binary-shaped pupil mask, was used. We improved the temperature stability by installing the coronagraph optics in a vacuum chamber, controlling the temperature of the optical bench, and covering the vacuum chamber with thermal insulation layers. We evaluated how much the PSF subtraction contributes to the high contrast observation by subtracting the images obtained through the coronagraph. We also carried out multi- band experiments in order to demonstrate a more realistic observa...

  20. Magnetized Moving Mesh Merger of a Carbon-Oxygen White Dwarf Binary

    E-Print Network [OSTI]

    Zhu, Chenchong; van Kerkwijk, Marten H; Chang, Philip

    2015-01-01T23:59:59.000Z

    White dwarf binary mergers are possible progenitors to a number of unusual stars and transient phenomena, including type Ia supernovae. To date, simulations of mergers have not included magnetic fields, even though they are believed to play a significant role in the evolution of the merger remnant. We simulated a 0.625 - 0.65 $M_{\\odot}$ carbon-oxygen white dwarf binary merger in the magnetohydrodynamic moving mesh code Arepo. Each white dwarf was given an initial dipole field with a surface value of $\\sim10^3$ G. As in simulations of merging double neutron star binaries, we find exponential field growth within Kelvin-Helmholtz instability-generated vortices during the coalescence of the two stars. The final field has complex geometry, and a strength $>10^{10}$ G at the center of the merger remnant. Its energy is $\\sim2\\times10^{47}$ ergs, $\\sim0.2$% of the remnant's total energy. The strong field likely influences further evolution of the merger remnant by providing a mechanism for angular momentum transfer ...

  1. Binary classification of items of interest in a repeatable process

    DOE Patents [OSTI]

    Abell, Jeffrey A.; Spicer, John Patrick; Wincek, Michael Anthony; Wang, Hui; Chakraborty, Debejyo

    2014-06-24T23:59:59.000Z

    A system includes host and learning machines in electrical communication with sensors positioned with respect to an item of interest, e.g., a weld, and memory. The host executes instructions from memory to predict a binary quality status of the item. The learning machine receives signals from the sensor(s), identifies candidate features, and extracts features from the candidates that are more predictive of the binary quality status relative to other candidate features. The learning machine maps the extracted features to a dimensional space that includes most of the items from a passing binary class and excludes all or most of the items from a failing binary class. The host also compares the received signals for a subsequent item of interest to the dimensional space to thereby predict, in real time, the binary quality status of the subsequent item of interest.

  2. Observational Techniques for Detecting Planets in Binary Systems

    E-Print Network [OSTI]

    Matthew W. Muterspaugh; Maciej Konacki; Benjamin F. Lane; Eric Pfahl

    2007-05-21T23:59:59.000Z

    Searches for planets in close binary systems explore the degree to which stellar multiplicity inhibits or promotes planet formation. There is a degeneracy between planet formation models when only systems with single stars are studied--several mechanisms appear to be able to produce such a final result. This degeneracy is lifted by searching for planets in binary systems; the resulting detections (or evidence of non-existence) of planets in binaries isolates which models may contribute to how planets form in nature. In this chapter, we consider observational efforts to detect planetary companions to binary stars in two types of hierarchical planet-binary configurations: first ``S-type'' planets which orbit just one of the stars, with the binary period being much longer than the planet's; second, ``P-type'' or circumbinary planets, where the planet simultaneously orbits both stars, and the planetary orbital period is much longer than that of the binary. The S-type planet finding techniques are different for binaries that can or cannot be spatially resolved. For wider systems, techniques reviewed include dualstar interferometric differential astrometry and precision radial velocities. Alternatively, unresolved binaries can be studied using modified dualstar "PHASES-style" differential astrometry or a modification of the radial velocity technique for composite spectra. Should a fortunately aligned--but still long period--binary be found, eclipse timing can also reveal the presence of S-type planets. Methods for detecting P-type planets include the composite-spectra variant of the radial velocity technique and eclipse timing.

  3. Binary versus non-binary information in real time series: empirical results and maximum-entropy matrix models

    E-Print Network [OSTI]

    Almog, Assaf

    2014-01-01T23:59:59.000Z

    The dynamics of complex systems, from financial markets to the brain, can be monitored in terms of time series of activity of their fundamental elements (such as stocks or neurons respectively). While the main focus of time series analysis is on the magnitude of temporal increments, a significant piece of information is encoded into the binary projection (i.e. the sign) of such increments. In this paper we provide further evidence of this by showing strong nonlinear relationships between binary and non-binary properties of financial time series. We then introduce an information-theoretic approach to the analysis of the binary signature of single and multiple time series. Through the definition of maximum-entropy ensembles of binary matrices, we quantify the information encoded into the simplest binary properties of real time series and identify the most informative property given a set of measurements. Our formalism is able to replicate the observed binary/non-binary relations very well, and to mathematically...

  4. Definitions Numbered Space

    E-Print Network [OSTI]

    Behmer, Spencer T.

    Definitions · Numbered Space ­ a single space marked with a number and reserved for a single permit 24/7 · Unnumbered Space ­ a space which can be used by any customer allowed to park in that lot. High Low Average Question 4: If I buy a staff permit for an UNNUMBERED* space in a non-gated surface

  5. Comment "On the statistics of the product of a Gaussian process and a pseudo random binary code" 

    E-Print Network [OSTI]

    Painter, John H.; Jacobs, I.

    1966-01-01T23:59:59.000Z

    908 PROCEEDINGS OF THE IEEE JUNE Comment "On the Statistics of the Product of a Gaussian Process and a Pseudo Random Binary Code" In a recent correspondence, Painter' shows that the first-order statistics of the product of a Gaussian noise... functions C(t) contain an infinite number of jump discontinuities; hence, almost all sample functions of Z(t) contain jump discontinuities. However, for a stationary Gaussian process, Manuscript received March 2.1966. 1 J. H. Painter. Proc. IEEE...

  6. Trajectories of the images in binary microlensing

    E-Print Network [OSTI]

    V. Bozza

    2001-05-16T23:59:59.000Z

    We study in detail the trajectories followed by single images during binary microlensing events. Starting from perturbative resolutions of the lens equation, we explore the full parameter space by continuity arguments. We see that the images created during the caustic crossing can recombine with the others in different ways. This leads to a new classification of the microlensing events according to the behaviour of the images. We show that the images involved in these combinations depend on the folds that are crossed at the entry and at the exit from the caustic. Non-trivial trajectories can be classified into four main types. Some consequences for the motion of the center of light of the source in astrometric measurements are also examined.

  7. Phase equilibrium measurements on nine binary mixtures

    SciTech Connect (OSTI)

    Wilding, W.V. [Brigham Young Univ., Provo, UT (United States). Chemical Engineering Dept.] [Brigham Young Univ., Provo, UT (United States). Chemical Engineering Dept.; Giles, N.F.; Wilson, L.C. [Wiltec Research Co. Inc., Provo, UT (United States)] [Wiltec Research Co. Inc., Provo, UT (United States)

    1996-11-01T23:59:59.000Z

    Phase equilibrium measurements have been performed on nine binary mixtures. The PTx method was used to obtain vapor-liquid equilibrium data for the following systems at two temperatures each: (aminoethyl)piperazine + diethylenetriamine; 2-butoxyethyl acetate + 2-butoxyethanol; 2-methyl-2-propanol + 2-methylbutane; 2-methyl-2-propanol + 2-methyl-2-butene; methacrylonitrile + methanol; 1-chloro-1,1-difluoroethane + hydrogen chloride; 2-(hexyloxy)ethanol + ethylene glycol; butane + ammonia; propionaldehyde + butane. Equilibrium vapor and liquid phase compositions were derived form the PTx data using the Soave equation of state to represent the vapor phase and the Wilson or the NRTL activity coefficient model to represent the liquid phase. A large immiscibility region exists in the butane + ammonia system at 0 C. Therefore, separate vapor-liquid-liquid equilibrium measurements were performed on this system to more precisely determine the miscibility limits and the composition of the vapor phase in equilibrium with the two liquid phases.

  8. Mapping the peculiar binary GP Com

    E-Print Network [OSTI]

    L. Morales-Rueda; T. R. Marsh; R. C. North

    2000-08-29T23:59:59.000Z

    We present high resolution spectra of the AM CVn helium binary GP Com at two different wavelength ranges. The spectra show the same flaring behaviour observed in previous UV and optical data. We find that the central spike contributes to the flare spectra indicating that its origin is probably the compact object. We also detect that the central spike moves with orbital phase following an S-wave pattern. The radial velocity semiamplitude of the S-wave is \\~10 km/s which indicates its origin is near the centre of mass of the system, which in this case lies very close to the white dwarf. The Stark effect seems to affect significantly the central spike of some of the lines suggesting that it forms in a high electron density region. This again favours the idea that the central spike originates in the white dwarf. We present Doppler maps obtained for the emission lines which show three clear emission regions.

  9. Mapping the peculiar binary GP Com

    E-Print Network [OSTI]

    Morales-Rueda, L; North, R C

    2000-01-01T23:59:59.000Z

    We present high resolution spectra of the AM CVn helium binary GP Com at two different wavelength ranges. The spectra show the same flaring behaviour observed in previous UV and optical data. We find that the central spike contributes to the flare spectra indicating that its origin is probably the compact object. We also detect that the central spike moves with orbital phase following an S-wave pattern. The radial velocity semiamplitude of the S-wave is \\~10 km/s which indicates its origin is near the centre of mass of the system, which in this case lies very close to the white dwarf. The Stark effect seems to affect significantly the central spike of some of the lines suggesting that it forms in a high electron density region. This again favours the idea that the central spike originates in the white dwarf. We present Doppler maps obtained for the emission lines which show three clear emission regions.

  10. Dynamical evolution of active detached binaries on log Jo - log M diagram and contact binary formation

    E-Print Network [OSTI]

    Z. Eker; O. Demircan; S. Bilir; Y. Karatas

    2006-09-14T23:59:59.000Z

    Orbital angular momentum (Jo), systemic mass (M) and orbital period (P) distributions of chromospherically active binaries (CAB) and W Ursae Majoris (W UMa) systems were investigated. The diagrams of log Jo - log P, log M - log P and log Jo-log M were formed from 119 CAB and 102 W UMa stars. The log Jo-log M diagram is found to be most meaningful in demonstrating dynamical evolution of binary star orbits. A slightly curved borderline (contact border) separating the detached and the contact systems was discovered on the log Jo - log M diagram. Since orbital size (a) and period (P) of binaries are determined by their current Jo, M and mass ratio q, the rates of orbital angular momentum loss (dlog Jo/dt) and mass loss (dlog M/dt) are primary parameters to determine the direction and the speed of the dynamical evolution. A detached system becomes a contact system if its own dynamical evolution enables it to pass the contact border on the log Jo - log M diagram. Evolution of q for a mass loosing detached system is unknown unless mass loss rate for each component is known. Assuming q is constant in the first approximation and using the mean decreasing rates of Jo and M from the kinematical ages of CAB stars, it has been predicted that 11, 23 and 39 cent of current CAB stars would transform to W UMa systems if their nuclear evolution permits them to live 2, 4 and 6 Gyrs respectively.

  11. A CHANGE IN THE LIGHT CURVE OF KUIPER BELT CONTACT BINARY (139775) 2001 QG{sub 298}

    SciTech Connect (OSTI)

    Lacerda, Pedro, E-mail: p.lacerda@qub.ac.uk [Astrophysics Research Centre, Queen's University Belfast, Belfast BT7 1NN (United Kingdom)

    2011-09-15T23:59:59.000Z

    New observations show that the light curve of Kuiper Belt contact binary (139775) 2001 QG{sub 298} has changed substantially since the first observations in 2003. The 2010 light curve has a peak-to-peak photometric range of {Delta}m{sub 2010} = 0.7 {+-} 0.1 mag, significantly lower than in 2003, {Delta}m{sub 2003} = 1.14 {+-} 0.04 mag. This change is most simply interpreted if 2001 QG{sub 298} has an obliquity near 90{sup 0}. The observed decrease in {Delta}m is caused by a change in viewing geometry, from equator-on in 2003 to nearly 16{sup 0} (the orbital angular distance covered by the object between the observations) off the equator in 2010. The 2003 and 2010 light curves have the same rotation period and appear in phase when shifted by an integer number of full rotations, also consistent with high obliquity. Based on the new 2010 light curve data, we find that 2001 QG{sub 298} has an obliquity of {epsilon} = 90{sup 0} {+-} 30{sup 0}. Current estimates of the intrinsic fraction of contact binaries in the Kuiper Belt are debiased assuming that these objects have randomly oriented spins. If, as 2001 QG2{sub 98}, Kuiper Belt Object contact binaries tend to have large obliquities, a larger correction is required. As a result, the abundance of contact binaries may be larger than previously believed.

  12. The dominant X-ray wind in massive star binaries

    E-Print Network [OSTI]

    J. M. Pittard; I. R. Stevens

    2002-04-15T23:59:59.000Z

    We investigate which shocked wind is responsible for the majority of the X-ray emission in colliding wind binaries, an issue where there is some confusion in the literature, and which we show is more complicated than has been assumed. We find that where both winds rapidly cool (typically close binaries), the ratio of the wind speeds is often more important than the momentum ratio, because it controls the energy flux ratio, and the faster wind is generally the dominant emitter. When both winds are largely adiabatic (typically long-period binaries), the slower and denser wind will cool faster and the stronger wind generally dominates the X-ray luminosity.

  13. Light and Life: Exotic Photosynthesis in Binary Star Systems

    E-Print Network [OSTI]

    O'Malley-James, J T; Cockell, C S; Greaves, J S

    2011-01-01T23:59:59.000Z

    The potential for hosting photosynthetic life on Earth-like planets within binary/multiple stellar systems was evaluated by modelling the levels of photosynthetically active radiation (PAR) such planets receive. Combinations of M and G stars in: (i) close-binary systems; (ii) wide-binary systems and (iii) three-star systems were investigated and a range of stable radiation environments found to be possible. These environmental conditions allow for the possibility of familiar, but also more exotic forms of photosynthetic life, such as infrared photosynthesisers and organisms specialised for specific spectral niches.

  14. Report number codes

    SciTech Connect (OSTI)

    Nelson, R.N. (ed.)

    1985-05-01T23:59:59.000Z

    This publication lists all report number codes processed by the Office of Scientific and Technical Information. The report codes are substantially based on the American National Standards Institute, Standard Technical Report Number (STRN)-Format and Creation Z39.23-1983. The Standard Technical Report Number (STRN) provides one of the primary methods of identifying a specific technical report. The STRN consists of two parts: The report code and the sequential number. The report code identifies the issuing organization, a specific program, or a type of document. The sequential number, which is assigned in sequence by each report issuing entity, is not included in this publication. Part I of this compilation is alphabetized by report codes followed by issuing installations. Part II lists the issuing organization followed by the assigned report code(s). In both Parts I and II, the names of issuing organizations appear for the most part in the form used at the time the reports were issued. However, for some of the more prolific installations which have had name changes, all entries have been merged under the current name.

  15. Green's functions and hydrodynamics for isotopic binary diffusion

    E-Print Network [OSTI]

    R. van Zon; E. G. D. Cohen

    2005-08-10T23:59:59.000Z

    We study classical binary fluid mixtures in which densities vary on very short time (ps) and length (nm) scales, such that hydrodynamics does not apply. In a pure fluid with a localized heat pulse the breakdown of hydrodynamics was overcome using Green's functions which connect the initial densities to those at later times. Numerically it appeared that for long times the results from the Green's functions would approach hydrodynamics. In this paper we extend the Green's functions theory to binary mixtures. For the case of isothermal isobaric mutual diffusion in isotopic binary mixtures and ideal binary mixtures, which is easier to handle than heat conduction yet still non-trivial, we show analytically that in the Green's function approach one recovers hydrodynamic behaviour at long time scales provided the system reaches local equilibrium at long times. This is a first step toward giving the Green's function theory a firmer basis because it can for this case be considered as an extension of hydrodynamics.

  16. High energy gamma-rays from massive binary systems

    E-Print Network [OSTI]

    W. Bednarek

    2008-06-27T23:59:59.000Z

    During last years a few massive binary systems have been detected in the TeV gamma-rays. This gamma-ray emission is clearly modulated with the orbital periods of these binaries suggesting its origin inside the binary system. In this paper we summarize the anisotropic IC e-p pair cascade model as likely explanation of these observations. We consider scenarios in which particles are accelerated to relativistic energies, either due to the presence of an energetic pulsar inside the binary, or as a result of accretion process onto the compact object during which the jet is launched from the inner part of the accretion disk, or in collisions of stellar winds from the massive companions.

  17. accuracy binary black: Topics by E-print Network

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    P. Uttley 2005-08-02 354 Black-Box Identification for PLC based MPC of a Binary Distillation Column Engineering Websites Summary: Black-Box Identification for PLC based MPC of...

  18. SOLIDIFICATION FRONTS AND SOLUTE TRAPPING IN A BINARY ALLOY

    E-Print Network [OSTI]

    Fife, Paul

    , Israel and PAUL C. FIFE , Mathematics Department, University of Utah, Salt Lake City, Utah 84112, USA­9703483. 1 #12;1 Introduction During the process of solidification of molten binary alloys

  19. Grain boundary segregation and thermodynamically stable binary nanocrystalline alloys

    E-Print Network [OSTI]

    Trelewicz, Jason R.

    A free-energy function for binary polycrystalline solid solutions is developed based on pairwise nearest-neighbor interactions. The model permits intergranular regions to exhibit unique energetics and compositions from ...

  20. Synthesis and characterization of nanocrystalline binary and ternary intermetallic compounds

    E-Print Network [OSTI]

    Leonard, Brian Matthew

    2009-05-15T23:59:59.000Z

    -technological applications has generated renewed interest in their synthesis. Current capabilities for synthesizing nanocrystalline materials are well-established for single metals and simple binary phases, but very few processes are capable of reliably producing...

  1. Optimization With Parity Constraints: From Binary Codes to Discrete Integration

    E-Print Network [OSTI]

    Bejerano, Gill

    Optimization With Parity Constraints: From Binary Codes to Discrete Integration Stefano Ermon guarantees on the quality of the solution found. Markov Chain Monte Carlo [17, 21, 32] and Importance

  2. A class of non-binary LDPC codes

    E-Print Network [OSTI]

    Gilra, Deepak

    2004-09-30T23:59:59.000Z

    A CLASS OF NON-BINARY LDPC CODES A Thesis by DEEPAK GILRA Submitted to the Office of Graduate Studies of Texas A&M University in partial fulfillment of the requirements for the degree of MASTER OF SCIENCE... May 2003 Major Subject: Electrical Engineering A CLASS OF NON-BINARY LDPC CODES A Thesis by DEEPAK GILRA Submitted to Texas A&M University in partial fulfillment of the requirements...

  3. Manifold corrections on spinning compact binaries

    SciTech Connect (OSTI)

    Zhong Shuangying; Wu Xin [Nanchang University, Nanchang 330031 (China)

    2010-05-15T23:59:59.000Z

    This paper deals mainly with a discussion of three new manifold correction methods and three existing ones, which can numerically preserve or correct all integrals in the conservative post-Newtonian Hamiltonian formulation of spinning compact binaries. Two of them are listed here. One is a new momentum-position scaling scheme for complete consistency of both the total energy and the magnitude of the total angular momentum, and the other is the Nacozy's approach with least-squares correction of the four integrals including the total energy and the total angular momentum vector. The post-Newtonian contributions, the spin effects, and the classification of orbits play an important role in the effectiveness of these six manifold corrections. They are all nearly equivalent to correct the integrals at the level of the machine epsilon for the pure Kepler problem. Once the third-order post-Newtonian contributions are added to the pure orbital part, three of these corrections have only minor effects on controlling the errors of these integrals. When the spin effects are also included, the effectiveness of the Nacozy's approach becomes further weakened, and even gets useless for the chaotic case. In all cases tested, the new momentum-position scaling scheme always shows the optimal performance. It requires a little but not much expensive additional computational cost when the spin effects exist and several time-saving techniques are used. As an interesting case, the efficiency of the correction to chaotic eccentric orbits is generally better than one to quasicircular regular orbits. Besides this, the corrected fast Lyapunov indicators and Lyapunov exponents of chaotic eccentric orbits are large as compared with the uncorrected counterparts. The amplification is a true expression of the original dynamical behavior. With the aid of both the manifold correction added to a certain low-order integration algorithm as a fast and high-precision device and the fast Lyapunov indicators of two nearby trajectories, phase space scans for chaos in the spinning compact binary system are given.

  4. Microlensing Binaries Discovered through High-Magnification Channel

    E-Print Network [OSTI]

    Shin, I -G; Park, S -Y; Han, C; Allen, W; Bos, M; Christie, G W; Depoy, D L; Dong, S; Drummond, J; Gal-Yam, A; Gaudi, B S; Gould, A; Hung, L -W; Janczak, J; Kaspi, S; Lee, C -U; Mallia, F; Maoz, D; Maury, A; McCormick, J; Monard, L A G; Moorhouse, D; Munoz, J A; Natusch, T; Nelson, C; Park, B -G; Pogge, R W; Polishook, D; Shvartzvald, Y; Shporer, A; Thornley, G; Yee, J C; Abe, F; Bennett, D P; Bond, I A; Botzler, C S; Fukui, A; Furusawa, K; Hayashi, F; Hearnshaw, J B; Hosaka, S; Itow, Y; Kamiya, K; Kilmartin, P M; Kobara, S; Korpela, A; Lin, W; Ling, C H; Makita, S; Masuda, K; Matsubara, Y; Miyake, N; Muraki, Y; Nagaya, M; Nishimoto, K; Ohnishi, K; Okumura, T; Omori, K; Perrott, Y C; Rattenbury, N; Saito, To; Skuljan, L; Sullivan, D J; Sumi, T; Suzuki, D; Sweatman, W L; Tristram, P J; Wada, K; Yock, P C M; Szymanski, M K; Kubiak, M; Pietrzynski, G; Soszynski, I; Szewczyk, O; Udalski, A; Ulaczyk, K; Wyrzykowski, L; Albrow, M D; Batista, V; Beaulieu, J -P; Brillant, S; Cassan, A; Cole, A; Corrales, E; Coutures, Ch; Dieters, S; Prester, D Dominis; Donatowicz, J; Fouque, P; Greenhill, J; Kane, S R; Menzies, J; Sahu, K C; Wambsganss, J; Williams, A; Zub, M; Allan, A; Bramich, D M; Browne, P; Dominik, M; Horne, K; Kains, N; Snodgrass, C; Steele, I; Street, R; Tsapras, Y; Bozza, V; Burgdorf, M J; Novati, S Calchi; Dreizler, S; Finet, F; Glitrup, M; Grundahl, F; Harpsoe, K; Hinse, T C; Hundertmark, M; Jorgensen, U G; Liebig, C; Maier, G; Mancini, L; Mathiasen, M; Rahvar, S; Ricci, D; Scarpetta, G; Skottfelt, J; Surdej, J; Southworth, J; Zimmer, F

    2011-01-01T23:59:59.000Z

    Microlensing can provide a useful tool to probe binary distributions down to low-mass limits of binary companions. In this paper, we analyze the light curves of 8 binary lensing events detected through the channel of high-magnification events during the seasons from 2007 to 2010. The perturbations, which are confined near the peak of the light curves, can be easily distinguished from the central perturbations caused by planets. However, the degeneracy between close and wide binary solutions cannot be resolved with a 3 \\sigma confidence level for 3 events, implying that the degeneracy would be an important obstacle in studying binary distributions. From investigating the dependence of the degeneracy on the lensing parameters, we find that the degeneracy becomes severe as the binary separation and the mass ratio deviate from the values of resonant caustics. The measured mass ratio of the event OGLE-2008-BLG-510/MOA-2008-BLG-369 is q~0.1, making the companion of the lens a strong brown-dwarf candidate.

  5. THE CLOSE BINARY FRACTION OF DWARF M STARS

    SciTech Connect (OSTI)

    Clark, Benjamin M. [Penn Manor High School, 100 East Cottage Avenue, Millersville, PA 17551 (United States); Blake, Cullen H.; Knapp, Gillian R. [Princeton University, Department of Astrophysical Sciences, Peyton Hall, Ivy Lane, Princeton, NJ 08544 (United States)

    2012-01-10T23:59:59.000Z

    We describe a search for close spectroscopic dwarf M star binaries using data from the Sloan Digital Sky Survey to address the question of the rate of occurrence of multiplicity in M dwarfs. We use a template-fitting technique to measure radial velocities from 145,888 individual spectra obtained for a magnitude-limited sample of 39,543 M dwarfs. Typically, the three or four spectra observed for each star are separated in time by less than four hours, but for {approx}17% of the stars, the individual observations span more than two days. In these cases we are sensitive to large-amplitude radial velocity variations on timescales comparable to the separation between the observations. We use a control sample of objects having observations taken within a four-hour period to make an empirical estimate of the underlying radial velocity error distribution and simulate our detection efficiency for a wide range of binary star systems. We find the frequency of binaries among the dwarf M stars with a < 0.4 AU to be 3%-4%. Comparison with other samples of binary stars demonstrates that the close binary fraction, like the total binary fraction, is an increasing function of primary mass.

  6. Mesoscale solubilization and critical phenomena in binary and quasi binary solutions of hydrotropes

    E-Print Network [OSTI]

    Andreas E. Robertson; Dung H. Phan; Joseph E. Macaluso; Vladimir N. Kuryakov; Elena V. Jouravleva; Christopher E. Bertrand; Igor K. Yudin; Mikhail A. Anisimov

    2015-03-24T23:59:59.000Z

    Hydrotropes are substances consisting of amphiphilic molecules that are too small to self assemble in equilibrium structures in aqueous solutions, but can form dynamic molecular clusters H bonded with water molecules. Some hydrotropes, such as low molecular weight alcohols and amines, can solubilize hydrophobic compounds in aqueous solutions at a mesoscopic scale, around 100 nm, with formation of long lived mesoscale droplets. In this work, we report on the studies of near critical and phase behavior of binary, 2,6-lutidine - H2O, and quasibinary, 2,6-lutidine - H2O - D2O, and tert-butanol - 2-butanol - H2O solutions in the presence of a solubilized hydrophobic impurity, cyclohexane. In additional to visual observation of fluid phase equilibria, two experimental techniques were used - light scattering and small - angle neutron scattering. It was found that the increase of the tert-butanol to 2-butanol ratio affects the liquid - liquid equilibria in the quasi-binary system at ambient pressure in the same way as the increase of pressure modifies the phase behavior of binary 2-butanol - H2O solutions. The correlation length of critical fluctuations near the liquid-liquid separation and the size of mesoscale droplets of solubilized cyclohexane were obtained by dynamic light scattering and by small - angle neutron scattering. It is shown that the effect of the presence of small amounts of cyclohexane on the near - critical phase behavior is twofold - the transition temperature changes towards increasing the two-phase domain, and long-lived mesoscopic inhomogeneities emerge in the macroscopically homogeneous domain. These homogeneities remain unchanged upon approach to the critical point of macroscopic phase separation and do not alter the universal nature of criticality. However, a larger amount of cyclohexane generates additional liquid-liquid phase separation at lower temperatures.

  7. A number of organizations,

    E-Print Network [OSTI]

    installed solar electric systems on a number of the city's buildings, including the Chicago Center for Green Technology shown here. CityofChicago Aggregated Purchasing--A Clean Energy Strategy SOLAR TODAY Aggregated Purchasing--A Clean Energy Strategy by Lori A. Bird and Edward A. Holt #12;November/December 2002 35 Power

  8. ALARA notes, Number 8

    SciTech Connect (OSTI)

    Khan, T.A.; Baum, J.W.; Beckman, M.C. [eds.] [eds.

    1993-10-01T23:59:59.000Z

    This document contains information dealing with the lessons learned from the experience of nuclear plants. In this issue the authors tried to avoid the `tyranny` of numbers and concentrated on the main lessons learned. Topics include: filtration devices for air pollution abatement, crack repair and inspection, and remote handling equipment.

  9. Molecular Design of Branched and Binary Molecules at Ordered Interfaces

    SciTech Connect (OSTI)

    Kirsten Larson Genson

    2005-12-27T23:59:59.000Z

    This study examined five different branched molecular architectures to discern the effect of design on the ability of molecules to form ordered structures at interfaces. Photochromic monodendrons formed kinked packing structures at the air-water interface due to the cross-sectional area mismatch created by varying number of alkyl tails and the hydrophilic polar head group. The lower generations formed orthorhombic unit cell with long range ordering despite the alkyl tails tilted to a large degree. Favorable interactions between liquid crystalline terminal groups and the underlying substrate were observed to compel a flexible carbosilane dendrimer core to form a compressed elliptical conformation which packed stagger within lamellae domains with limited short range ordering. A twelve arm binary star polymer was observed to form two dimensional micelles at the air-water interface attributed to the higher polystyrene block composition. Linear rod-coil molecules formed a multitude of packing structures at the air-water interface due to the varying composition. Tree-like rod-coil molecules demonstrated the ability to form one-dimensional structures at the air-water interface and at the air-solvent interface caused by the preferential ordering of the rigid rod cores. The role of molecular architecture and composition was examined and the influence chemically competing fragments was shown to exert on the packing structure. The amphiphilic balance of the different molecular series exhibited control on the ordering behavior at the air-water interface and within bulk structures. The shell nature and tail type was determined to dictate the preferential ordering structure and molecular reorganization at interfaces with the core nature effect secondary.

  10. Phase Transformations in Binary Colloidal Monolayers

    E-Print Network [OSTI]

    Ye Yang; Lin Fu; Catherine Marcoux; Joshua E. S. Socolar; Patrick Charbonneau; Benjamin B. Yellen

    2015-02-10T23:59:59.000Z

    Phase transformations can be difficult to characterize at the microscopic level due to the inability to directly observe individual atomic motions. Model colloidal systems, by contrast, permit the direct observation of individual particle dynamics and of collective rearrangements, which allows for real-space characterization of phase transitions. Here, we study a quasi-two-dimensional, binary colloidal alloy that exhibits liquid-solid and solid-solid phase transitions, focusing on the kinetics of a diffusionless transformation between two crystal phases. Experiments are conducted on a monolayer of magnetic and nonmagnetic spheres suspended in a thin layer of ferrofluid and exposed to a tunable magnetic field. A theoretical model of hard spheres with point dipoles at their centers is used to guide the choice of experimental parameters and characterize the underlying materials physics. When the applied field is normal to the fluid layer, a checkerboard crystal forms; when the angle between the field and the normal is sufficiently large, a striped crystal assembles. As the field is slowly tilted away from the normal, we find that the transformation pathway between the two phases depends strongly on crystal orientation, field strength, and degree of confinement of the monolayer. In some cases, the pathway occurs by smooth magnetostrictive shear, while in others it involves the sudden formation of martensitic plates.

  11. Diffusion and Interdiffusion in Binary Metallic Melts

    E-Print Network [OSTI]

    P. Kuhn; J. Horbach; F. Kargl; A. Meyer; Th. Voigtmann

    2014-08-09T23:59:59.000Z

    We discuss the dependence of self- and interdiffusion coefficients on temperature and composition for two prototypical binary metallic melts, Al-Ni and Zr-Ni, in molecular-dynamics (MD) computer simulations and the mode-coupling theory of the glass transition (MCT). Dynamical processes that are mainly entropic in origin slow down mass transport (as expressed through self diffusion) in the mixture as compared to the ideal-mixing contribution. Interdiffusion of chemical species is a competition of slow kinetic modes with a strong thermodynamic driving force that is caused by non-entropic interactions. The combination of both dynamic and thermodynamic effects causes qualitative differences in the concentration dependence of self-diffusion and interdiffusion coefficients. At high temperatures, the thermodynamic enhancement of interdiffusion prevails, while at low temperatures, kinetic effects dominate the concentration dependence, rationalized within MCT as the approach to its ideal-glass transition temperature $T_c$. The Darken equation relating self- and interdiffusion qualitatively reproduces the concentration-dependence in both Zr-Ni and Al-Ni, but quantitatively, the kinetic contributions to interdiffusion can be slower than the lower bound suggested by the Darken equation. As temperature is decreased, the agreement with Darken's equation improves, due to a strong coupling of all kinetic modes that is a generic feature predicted by MCT.

  12. The Connection Between Low-Mass X-ray Binaries and (Millisecond) Pulsars: A Binary Evolution Perspective

    E-Print Network [OSTI]

    Christopher J. Deloye

    2007-10-01T23:59:59.000Z

    I review the evolutionary connection between low-mass X-ray binaries (LMXBs) and pulsars with binary companions (bPSRs) from a stellar binary evolution perspective. I focus on the evolution of stellar binaries with end-states consisting of a pulsar with a low-mass (<1.0 solar mass) companion, starting at the point the companion's progenitor first initiates mass transfer onto the neutron star. Whether this mass transfer is stable and the physics driving ongoing mass transfer partitions the phase space of the companions's initial mass and initial orbital period into five regions. The qualitative nature of the mass-transfer process and the binary's final end-state differ between systems in each region; four of these regions each produce a particular class of LMXBs. I compare the theoretical expectations to the populations of galactic field LMXBs with companion-mass constraints and field bPSRs. I show that the population of accreting millisecond pulsars are all identified with only two of the four LMXB classes and that these systems do not have readily identifiable progeny in the bPSR population. I discuss which sub-populations of bPSRs can be explained by binary evolution theory and those that currently are not. Finally I discuss some outstanding questions in this field.

  13. Distinguishing types of compact-object binaries using the gravitational-wave signatures of their mergers

    E-Print Network [OSTI]

    Ilya Mandel; Carl-Johan Haster; Michal Dominik; Krzysztof Belczynski

    2015-05-04T23:59:59.000Z

    We analyze the distinguishability of populations of coalescing binary neutron stars, neutron-star black-hole binaries, and binary black holes, whose gravitational-wave signatures are expected to be observed by the advanced network of ground-based interferometers LIGO and Virgo. We consider population-synthesis predictions for plausible merging binary distributions in mass space, along with measurement accuracy estimates from the main gravitational-wave parameter-estimation pipeline. We find that for our model compact-object binary mass distribution, we can always distinguish binary neutron stars and black-hole--neutron-star binaries, but not necessarily black-hole--neutron-star binaries and binary black holes; however, with a few tens of detections, we can accurately identify the three subpopulations and measure their respective rates.

  14. Radial Velocity Studies of Close Binary Stars. XI

    E-Print Network [OSTI]

    Theodor Pribulla; Slavek M. Rucinski; Wenxian Lu; Stefan W. Mochnacki; George Conidis; R. M. Blake; Heide DeBond; J. R. Thomson; Wojtek Pych; Waldemar Ogloza; Michal Siwak

    2006-05-15T23:59:59.000Z

    Radial-velocity measurements and sine-curve fits to the orbital radial velocity variations are presented for ten close binary systems: DU Boo, ET Boo, TX Cnc, V1073 Cyg, HL Dra, AK Her, VW LMi, V566 Oph, TV UMi and AG Vir. By this contribution, the DDO program has reached the point of 100 published radial velocity orbits. The radial velocities have been determined using an improved fitting technique which uses rotational profiles to approximate individual peaks in broadening functions. Three systems, ET Boo, VW LMi and TV UMi, were found to be quadruple while AG Vir appears to be a spectroscopic triple. ET Boo, a member of a close visual binary with $P_{vis} = 113$ years, was previously known to be a multiple system, but we show that the second component is actually a close, non-eclipsing binary. The new observations enabled us to determine the spectroscopic orbits of the companion, non-eclipsing pairs in ET Boo and VW LMi. The particularly interesting case is VW LMi, where the period of the mutual revolution of the two spectroscopic binaries is only 355 days. While most of the studied eclipsing pairs are contact binaries, ET Boo is composed of two double-lined detached binaries and HL Dra is single-lined detached or semi-detached system. Five systems of this group were observed spectroscopically before: TX Cnc, V1073 Cyg, AK Her (as a single-lined binary), V566 Oph, AG Vir, but our new data are of much higher quality than the previous studies.

  15. A Spectroscopic Study of Mass Outflows in the Interacting Binary RY Scuti

    E-Print Network [OSTI]

    E. D. Grundstrom; D. R. Gies; T. C. Hillwig; M. V. McSwain; N. Smith; R. D. Gehrz; O. Stahl; A. Kaufer

    2007-06-21T23:59:59.000Z

    The massive interacting binary RY Scuti is an important representative of an active mass-transferring system that is changing before our eyes and which may be an example of the formation of a Wolf-Rayet star through tidal stripping. Utilizing new and previously published spectra, we present examples of how a number of illustrative absorption and emission features vary during the binary orbit. We identify spectral features associated with each component, calculate a new, double-lined spectroscopic binary orbit, and find masses of 7.1 +/- 1.2 M_sun for the bright supergiant and 30.0 +/- 2.1 M_sun for the hidden massive companion. Through tomographic reconstruction of the component spectra from the composite spectra, we confirm the O9.7 Ibpe spectral class of the bright supergiant and discover a B0.5 I spectrum associated with the hidden massive companion; however, we suggest that the latter is actually the spectrum of the photosphere of the accretion torus immediately surrounding the massive companion. We describe the complex nature of the mass loss flows from the system in the context of recent hydrodynamical models for beta Lyr, leading us to conclude RY Scuti has matter leaving the system in two ways: 1) a bipolar outflow from winds generated by the hidden massive companion, and 2) mass from the bright O9.7 Ibpe supergiant flowing from the region near the L2 point to fill out a large, dense circumbinary disk. This circumbinary disk (radius ~ 1 AU) may feed the surrounding double-toroidal nebula (radius ~ 2000 AU).

  16. Maximally Random Jamming of Two-Dimensional One-Component and Binary Hard Disc Fluids

    E-Print Network [OSTI]

    Xinliang Xu; Stuart A. Rice

    2010-10-05T23:59:59.000Z

    We report calculations of the density of maximally random jamming (aka random close packing) of one-component and binary hard disc fluids. The theoretical structure used provides a common framework for description of the hard disc liquid to hexatic, the liquid to hexagonal crystal and the liquid-to-maximally random jammed state transitions. Our analysis is based on locating a particular bifurcation of the solutions of the integral equation for the inhomogeneous single particle density at the transition between different spatial structures. The bifurcation of solutions we study is initiated from the dense metastable fluid, and we associate it with the limit of stability of the fluid, which we identify with the transition from the metastable fluid to a maximally random jammed state. For the one-component hard disc fluid the predicted packing fraction at which the metastable fluid to maximally random jammed state transition occurs is 0.84, in excellent agreement with the experimental value 0.84 \\pm 0.02. The corresponding analysis of the limit of stability of a binary hard disc fluid with specified disc diameter ratio and disc composition requires extra approximations in the representations of the direct correlation function, the equation of state, and the number of order parameters accounted for. Keeping only the order parameter identified with the largest peak in the structure factor of the highest density regular lattice with the same disc diameter ratio and disc composition as the binary fluid, the predicted density of maximally random jamming is found to be 0.84 to 0.87, depending on the equation of state used, and very weakly dependent on the ratio of disc diameters and the fluid composition, in agreement with both experimental data and computer simulation data.

  17. Formation of contact in massive close binaries

    E-Print Network [OSTI]

    S. Wellstein; N. Langer; H. Braun

    2001-02-14T23:59:59.000Z

    We present evolutionary calculations for 74 close binaries systems with initial primary masses in the range 12...25 M_sun, and initial secondary masses between 6 and 24 M_sun. The initial periods were chosen such that mass overflow starts during the core hydrogen burning phase of the primary (Case A), or shortly thereafter (Case B). We assume conservative evolution for contact-free systems, i.e., no mass or angular momentum loss from those system except due to stellar winds. We investigate the borderline between contact-free evolution and contact, as a function of the initial system parameters. We also investigate the effect of the treatment of convection, and found it relevant for contact and supernova order in Case A systems, particularly for the highest considered masses. For Case B systems we find contact for initial periods above approximate 10 days and below. However, in that case (and for not too large periods) contact occurs only after the mass ratio has been reversed, due to the increased fraction of the donor's convective envelope. As most In all Cases we find contact for mass ratios below approximate 0.65. We derive the observable properties of our systems after the major mass transfer event, where the mass gainer is a main sequence or supergiant O or early B type star, and the mass loser is a helium star. We point out that the assumption of conservative evolution for contact-free systems could be tested by finding helium star companions to O stars.

  18. Spectroscopic Binaries in Globular Clusters. I. A Search for Ultra-Hard Binaries on the Main Sequence in M4

    E-Print Network [OSTI]

    Patrick Cote; Phil Fischer

    1996-05-02T23:59:59.000Z

    A search for spectroscopic binaries on the main sequence of the nearby globular cluster M4 has been undertaken with Argus, the multi-object spectrograph on the CTIO 4.0m telescope. A pair of radial velocities (median precision $\\simeq$ 2 km/s) separated by 11 months have been obtained for 33 turnoff dwarfs in the magnitude range 16.9 $\\le$ V $\\le$ 17.4. Monte-Carlo simulations have been used to derive a binary fraction, X, for systems with periods in the range 2 days $\\lae {\\rm P} \\lae$ 3 years and mass ratios between 0.2 and 1.0. This short-period cutoff is more than an order of magnitude smaller than those of existing radial velocity surveys and is comparable to the shortest periods possible for main-sequence turnoff stars. Our survey therefore provides a first glimpse into the abundance of ``ultra-hard" spectroscopic binaries in globular clusters. Although no star shows a velocity variation larger than 14 km/s, two objects are observed to have chi-square probabilities below 0.1\\%. No such stars are expected in a sample of 33. We find a best-fit binary fraction of X $\\simeq$ 0.15, a value which is consistent with recent estimates based on deep HST color-magnitude diagrams, as well as with the binary fraction of X $\\simeq$ 0.1 for nearby solar-type stars having similar periods and mass ratios. Our derived binary fraction suggests that exchange interactions with pre-existing binaries are a plausible means of explaining the origin of the hierarchical triple system containing the pulsar PSR 1620-26.

  19. Constraining the mass transfer in massive binaries through progenitor evolution models of Wolf-Rayet+O binaries

    E-Print Network [OSTI]

    Jelena Petrovic; Norbert Langer; Karel A. van der hucht

    2005-04-11T23:59:59.000Z

    Since close WR+O binaries are the result of a strong interaction of both stars in massive close binary systems, they can be used to constrain the highly uncertain mass and angular momentum budget during the major mass transfer phase. We explore the progenitor evolution of the three best suited WR+O binaries HD 90657, HD 186943 and HD 211853, which are characterized by a WR/O mass ratio of $\\sim$0.5 and periods of 6..10 days. We are doing so at three different levels of approximation: predicting the massive binary evolution through simple mass loss and angular momentum loss estimates, through full binary evolution models with parametrized mass transfer efficiency, and through binary evolution models including rotation of both components and a physical model which allows to compute mass and angular momentum loss from the binary system as function of time during the mass transfer process. All three methods give consistently the same answers. Our results show that, if these systems formed through stable mass transfer, their initial periods were smaller than their current ones, which implies that mass transfer has started during the core hydrogen burning phase of the initially more massive star. Furthermore, the mass transfer in all three cases must have been highly non-conservative, with on average only $\\sim$10% of the transferred mass being retained by the mass receiving star. This result gives support to our system mass and angular momentum loss model, which predicts that, in the considered systems, about 90% of the overflowing matter is expelled by the rapid rotation of the mass receiver close to the $\\Omega$-limit, which is reached through the accretion of the remaining 10%.

  20. NSR Key Number Retrieval

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOE Office of Science (SC)Integrated CodesTransparency VisitSilver Toyota PriusNSR Key Number Retrieval Pease

  1. Gamma-ray emission from binaries in context

    E-Print Network [OSTI]

    Dubus, Guillaume

    2015-01-01T23:59:59.000Z

    More than a dozen binary systems are now established as sources of variable, high energy (HE, 0.1-100 GeV) gamma rays. Five are also established sources of very high energy (VHE, >100 GeV) gamma rays. The mechanisms behind gamma-ray emission in binaries are very diverse. My current understanding is that they divide up into four types of systems: gamma-ray binaries, powered by pulsar rotation; microquasars, powered by accretion onto a black hole or neutron star; novae, powered by thermonuclear runaway on a white dwarf; colliding wind binaries, powered by stellar winds from massive stars. Some of these types had long been suspected to emit gamma rays (microquasars), others have taken the community by surprise (novae). My purpose here is to provide a brief review of the current status of gamma-ray emission from binaries, in the context of related objects where similar mechanisms are at work (pulsar wind nebulae, active galactic nuclei, supernova remnants).

  2. Mergers of binary neutron stars with realistic spin

    E-Print Network [OSTI]

    Sebastiano Bernuzzi; Tim Dietrich; Wolfgang Tichy; Bernd Bruegmann

    2014-06-06T23:59:59.000Z

    Simulations of binary neutron stars have seen great advances in terms of physical detail and numerical quality. However, the spin of the neutron stars, one of the simplest global parameters of binaries, remains mostly unstudied. We present the first, fully nonlinear general relativistic dynamical evolutions of the last three orbits for constraint satisfying initial data of spinning neutron star binaries, with astrophysically realistic spins aligned and anti-aligned to the orbital angular momentum. The initial data is computed with the constant rotational velocity approach. The dynamics of the systems is analyzed in terms of gauge-invariant binding energy vs. orbital angular momentum curves. By comparing to a binary black hole configuration we can estimate the different tidal and spin contributions to the binding energy for the first time. First results on the gravitational wave forms are presented. The phase evolution during the orbital motion is significantly affected by spin-orbit interactions, leading to delayed or early mergers. Furthermore, a frequency shift in the main emission mode of the hyper massive neutron star is observed. Our results suggest that a detailed modeling of merger waveforms requires the inclusion of spin, even for the moderate magnitudes observed in binary neutron star systems.

  3. The DWARF project: Eclipsing binaries - precise clocks to discover exoplanets

    E-Print Network [OSTI]

    Pribulla, T; von Eiff, M Ammler -; Andreev, M; Aslantürk, A; Awadalla, N; Balu?anský, D; Bonanno, A; Boži?, H; Catanzaro, G; Çelik, L; Christopoulou, P E; Covino, E; Cusano, F; Dimitrov, D; Dubovský, P; Esmer, E M; Frasca, A; Hambálek, ?; Hanna, M; Hanslmeier, A; Kalomeni, B; Kjurkchieva, D P; Krushevska, V; Kudzej, I; Kundra, E; Kuznyetsova, Yu; Lee, J W; Leitzinger, M; Maciejewski, G; Moldovan, D; Morais, M H M; Mugrauer, M; Neuhäuser, R; Niedzielski, A; Odert, P; Ohlert, J; Özavc?, ?; Papageorgiou, A; Parimucha, Š; Poddaný, S; Pop, A; Raetz, M; Raetz, S; Romanyuk, Ya; Ruždjak, D; Schulz, J; ?enavc?, H V; Szalai, T; Székely, P; Sudar, D; Tezcan, C T; Törün, M E; Turcu, V; Vince, O; Zejda, M

    2012-01-01T23:59:59.000Z

    We present a new observational campaign, DWARF, aimed at detection of circumbinary extrasolar planets using the timing of the minima of low-mass eclipsing binaries. The observations will be performed within an extensive network of relatively small to medium-size telescopes with apertures of ~20-200 cm. The starting sample of the objects to be monitored contains (i) low-mass eclipsing binaries with M and K components, (ii) short-period binaries with sdB or sdO component, and (iii) post-common-envelope systems containing a WD, which enable to determine minima with high precision. Since the amplitude of the timing signal increases with the orbital period of an invisible third component, the timescale of project is long, at least 5-10 years. The paper gives simple formulas to estimate suitability of individual eclipsing binaries for the circumbinary planet detection. Intrinsic variability of the binaries (photospheric spots, flares, pulsation etc.) limiting the accuracy of the minima timing is also discussed. The...

  4. Dynamical resonance locking in tidally interacting binary systems

    E-Print Network [OSTI]

    Joshua Burkart; Eliot Quataert; Phil Arras

    2014-10-25T23:59:59.000Z

    We examine the dynamics of resonance locking in detached, tidally interacting binary systems. In a resonance lock, a given stellar or planetary mode is trapped in a highly resonant state for an extended period of time, during which the spin and orbital frequencies vary in concert to maintain the resonance. This phenomenon is qualitatively similar to resonance capture in planetary dynamics. We show that resonance locks can accelerate the course of tidal evolution in eccentric systems and also efficiently couple spin and orbital evolution in circular binaries. Previous analyses of resonance locking have not treated the mode amplitude as a fully dynamical variable, but rather assumed the adiabatic (i.e. Lorentzian) approximation valid only in the limit of relatively strong mode damping. We relax this approximation, analytically derive conditions under which the fixed point associated with resonance locking is stable, and further check these analytic results using numerical integrations of the coupled mode, spin, and orbital evolution equations. These show that resonance locking can sometimes take the form of complex limit cycles or even chaotic trajectories. We provide simple analytic formulae that define the binary and mode parameter regimes in which resonance locks of some kind occur (stable, limit cycle, or chaotic). We briefly discuss the astrophysical implications of our results for white dwarf and neutron star binaries as well as eccentric stellar binaries.

  5. Grant Application Package CFDA Number

    E-Print Network [OSTI]

    Talley, Lynne D.

    Grant Application Package CFDA Number: Opportunity Title: Offering Agency: Agency Contact: Opportunity Open Date: Opportunity Close Date: CFDA Description: Opportunity Number: Competition ID

  6. A PRECISE MASS MEASUREMENT OF THE INTERMEDIATE-MASS BINARY PULSAR PSR J1802 - 2124

    SciTech Connect (OSTI)

    Ferdman, R. D.; Cognard, I.; Desvignes, G.; Theureau, G. [Station de Radioastronomie de Nancay, Observatoire de Paris, 18330 Nancay (France); Stairs, I. H. [Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1 (Canada); Kramer, M. [Max-Planck-Institut fuer Radioastronomie, Auf dem Huegel 69, 53121, Bonn (Germany); McLaughlin, M. A.; Lorimer, D. R. [Department of Physics, West Virginia University, Morgantown, WV 26505 (United States); Nice, D. J. [Physics Department, Bryn Mawr College, Bryn Mawr, PA 19010 (United States); Manchester, R. N.; Hobbs, G. [Australia Telescope National Facility, CSIRO, Epping, NSW 1710 (Australia); Lyne, A. G.; Faulkner, A. [Jodrell Bank Centre for Astrophysics, University of Manchester, Alan Turing Building, Oxford Road, Manchester M13 9PL (United Kingdom); Camilo, F. [Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027 (United States); Possenti, A. [INAF, Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, 09012 Capoterra (Italy); Demorest, P. B. [National Radio Astronomy Observatory, Charlottesville, VA 22901 (United States); Backer, D. C., E-mail: robert.ferdman@obs-nancay.f [Department of Astronomy and Radio Astronomy Laboratory, University of California, Berkeley, CA 94720 (United States)

    2010-03-10T23:59:59.000Z

    PSR J1802 - 2124 is a 12.6 ms pulsar in a 16.8 hr binary orbit with a relatively massive white dwarf (WD) companion. These properties make it a member of the intermediate-mass class of binary pulsar (IMBP) systems. We have been timing this pulsar since its discovery in 2002. Concentrated observations at the Green Bank Telescope, augmented with data from the Parkes and Nancay observatories, have allowed us to determine the general relativistic Shapiro delay. This has yielded pulsar and WD mass measurements of 1.24 +- 0.11 M{sub sun} and 0.78 +- 0.04 M{sub sun} (68% confidence), respectively. The low mass of the pulsar, the high mass of the WD companion, the short orbital period, and the pulsar spin period may be explained by the system having gone through a common-envelope phase in its evolution. We argue that selection effects may contribute to the relatively small number of known IMBPs.

  7. PROBING ELECTRON-CAPTURE SUPERNOVAE: X-RAY BINARIES IN STARBURSTS

    SciTech Connect (OSTI)

    Linden, T. [Department of Physics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064 (United States); Sepinsky, J. F. [Department of Physics and Electrical Engineering, University of Scranton, Scranton, PA 18510 (United States); Kalogera, V. [Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208 (United States); Belczynski, K. [Los Alamos National Laboratory, Los Alamos, NM 87545 (United States)

    2009-07-10T23:59:59.000Z

    We develop population models of high-mass X-ray binaries (HMXBs) formed after bursts of star formation and we investigate the effect of electron-capture supernovae (ECS) of massive ONeMg white dwarfs and the hypothesis that ECS events are associated with typically low supernova kicks imparted to the nascent neutron stars. We identify an interesting ECS bump in the time evolution of HMXB numbers; this bump is caused by significantly increased production of wind-fed HMXBs 20-60 Myr post-starburst. The amplitude and age extent of the ECS bump depend on the strength of ECS kicks and the mass range of ECS progenitors. We also find that ECS-HMXBs form through a specific evolutionary channel that is expected to lead to binaries with Be donors in wide orbits. These characteristics, along with their sensitivity to ECS properties, provide us with an intriguing opportunity to probe ECS physics and progenitors through studies of starbursts of different ages. Specifically, the case of the Small Magellanic Cloud, with a significant observed population of Be-HMXBs and starburst activity 30-60 Myr ago, arises as a promising laboratory for understanding the role of ECS in neutron star formation.

  8. Discovery of Two New Thermally Bloated Low-Mass White Dwarfs Among the Kepler Binaries

    E-Print Network [OSTI]

    Rappaport, S; Levine, A; Sanchis-Ojeda, R; Gandolfi, D; Nowak, G; Palle, E; Prsa, A

    2015-01-01T23:59:59.000Z

    We report the discovery of two new low-mass, thermally bloated, hot white dwarfs among the Kepler sample of eclipsing binaries. These are KIC 9164561 and KIC 10727668 with orbital periods of 1.2670 and 2.3058 days, respectively. The current primary in both systems is an A star of about 2 Msun. This brings the number of similar binaries among the Kepler sample to six, and the two new systems have the shortest orbital periods among them. The white dwarf in KIC 9164561 has the largest thermal bloating, compared to its cold degenerate radius, of about a factor of 14. We utilize RV measurements of the A star in KIC 9164561 to determine the white dwarf mass rather accurately: 0.197 +/- 0.005 Msun. The mass of the white dwarf in KIC 10727668 is based on the Doppler boosting signal in the Kepler photometry, and is less accurately determined to be 0.266 +/- 0.035 Msun. Based on the inferred radii and effective temperatures of these two white dwarfs we are able to make an independent theoretical estimate of their masse...

  9. Mining Binary Expressions: Applications and Toon Calders

    E-Print Network [OSTI]

    Antwerpen, Universiteit

    ,pareda}@uia.ua.ac.be Technical report TR0008, June 2000 Abstract In data mining, searching for frequent patterns is a common exponentially large, we use data mining techniques to avoid expo- nential execution times. We present results of the number of partial orders 22 B Example run of the algorithm 24 2 #12;1 Introduction In data mining

  10. Photometric study of the pulsating, eclipsing binary OO DRA

    SciTech Connect (OSTI)

    Zhang, X. B.; Deng, L. C.; Tian, J. F.; Wang, K.; Yan, Z. Z.; Luo, C. Q. [Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China); Sun, J. J.; Liu, Q. L.; Xin, H. Q.; Zhou, Q. [Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008 (China); Luo, Z. Q. [Department of Physics, China West Normal University, Nanchong 637002 (China)

    2014-12-01T23:59:59.000Z

    We present a comprehensive photometric study of the pulsating, eclipsing binary OO Dra. Simultaneous B- and V-band photometry of the star was carried out on 14 nights. A revised orbital period and a new ephemeris were derived from the data. The first photometric solution of the binary system and the physical parameters of the component stars are determined. They reveal that OO Dra could be a detached system with a less-massive secondary component nearly filling its Roche lobe. By subtracting the eclipsing light changes from the data, we obtained the intrinsic pulsating light curves of the hotter, massive primary component. A frequency analysis of the residual light yields two confident pulsation modes in both B- and V-band data with the dominant frequency detected at 41.865 c/d. A brief discussion concerning the evolutionary status and the pulsation nature of the binary system is finally given.

  11. Grant Title: KNOWLEDGE DISSEMINATION CONFERENCE GRANTS PROGRAM ANNOUNCEMENT Funding Opportunity Number: CFDA Number(s) -93.243; Funding Opportunity Number -OA-08-002.

    E-Print Network [OSTI]

    Farritor, Shane

    Number: CFDA Number(s) - 93.243; Funding Opportunity Number - OA-08-002. Agency/Department: Department

  12. COMPACT BINARY PROGENITORS OF SHORT GAMMA-RAY BURSTS

    SciTech Connect (OSTI)

    Giacomazzo, Bruno [JILA, University of Colorado and National Institute of Standards and Technology, Boulder, CO 80309 (United States); Perna, Rosalba [JILA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309 (United States); Rezzolla, Luciano [Max-Planck-Institut fuer Gravitationsphysik, Albert-Einstein-Institut, Potsdam D-14476 (Germany); Troja, Eleonora [NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Lazzati, Davide [Department of Physics, NC State University, 2401 Stinson Drive, Raleigh, NC 27695-8202 (United States)

    2013-01-10T23:59:59.000Z

    In recent years, detailed observations and accurate numerical simulations have provided support to the idea that mergers of compact binaries containing either two neutron stars (NSs) or an NS and a black hole (BH) may constitute the central engine of short gamma-ray bursts (SGRBs). The merger of such compact binaries is expected to lead to the production of a spinning BH surrounded by an accreting torus. Several mechanisms can extract energy from this system and power the SGRBs. Here we connect observations and numerical simulations of compact binary mergers, and use the current sample of SGRBs with measured energies to constrain the mass of their powering tori. By comparing the masses of the tori with the results of fully general-relativistic simulations, we are able to infer the properties of the binary progenitors that yield SGRBs. By assuming a constant efficiency in converting torus mass into jet energy, {epsilon}{sub jet} = 10%, we find that most of the tori have masses smaller than 0.01 M{sub Sun }, favoring 'high-mass' binary NSs mergers, i.e., binaries with total masses {approx}> 1.5 the maximum mass of an isolated NS. This has important consequences for the gravitational wave signals that may be detected in association with SGRBs, since 'high-mass' systems do not form a long-lived hypermassive NS after the merger. While NS-BH systems cannot be excluded to be the engine of at least some of the SGRBs, the BH would need to have an initial spin of {approx}0.9 or higher.

  13. Accurate evolutions of unequal-mass neutron-star binaries: properties of the torus and short GRB engines

    E-Print Network [OSTI]

    Luciano Rezzolla; Luca Baiotti; Bruno Giacomazzo; David Link; Jose A. Font

    2010-05-13T23:59:59.000Z

    We present new results from accurate and fully general-relativistic simulations of the coalescence of unmagnetized binary neutron stars with various mass ratios. The evolution of the stars is followed through the inspiral phase, the merger and prompt collapse to a black hole, up until the appearance of a thick accretion disk, which is studied as it enters and remains in a regime of quasi-steady accretion. Although a simple ideal-fluid equation of state with \\Gamma=2 is used, this work presents a systematic study within a fully general relativistic framework of the properties of the resulting black-hole--torus system produced by the merger of unequal-mass binaries. More specifically, we show that: (1) The mass of the torus increases considerably with the mass asymmetry and equal-mass binaries do not produce significant tori if they have a total baryonic mass M_tot >~ 3.7 M_sun; (2) Tori with masses M_tor ~ 0.2 M_sun are measured for binaries with M_tot ~ 3.4 M_sun and mass ratios q ~ 0.75-0.85; (3) The mass of the torus can be estimated by the simple expression M_tor(q, M_tot) = [c_1 (1-q) + c_2](M_max-M_tot), involving the maximum mass for the binaries and coefficients constrained from the simulations, and suggesting that the tori can have masses as large as M_tor ~ 0.35 M_sun for M_tot ~ 2.8 M_sun and q ~ 0.75-0.85; (4) Using a novel technique to analyze the evolution of the tori we find no evidence for the onset of non-axisymmetric instabilities and that very little, if any, of their mass is unbound; (5) Finally, for all the binaries considered we compute the complete gravitational waveforms and the recoils imparted to the black holes, discussing the prospects of detection of these sources for a number of present and future detectors.

  14. Radar Imaging and Characterization of Binary Near-Earth Asteroid (185851) 2000 DP107

    E-Print Network [OSTI]

    2015-01-01T23:59:59.000Z

    modeling of triple near-Earth Asteroid (136617) 1994 CC.CHARACTERIZATION OF BINARY NEAR-EARTH ASTEROID (185851) 2000of Contact Binary Near-Earth Asteroids. In AAS/Division for

  15. 13 New Eclipsing Binaries with Additional Variability in the ASAS Catalogue

    E-Print Network [OSTI]

    B. Pilecki; D. M. Szczygie?

    2007-05-11T23:59:59.000Z

    We present 13 new ASAS eclipsing binaries that exhibit additional periodic variability due to pulsations, eclipses with another period or spots. All contact and semi-detached binaries from the ASAS Catalogue were investigated.

  16. Optical simulation of neutrino oscillations in binary waveguide arrays

    E-Print Network [OSTI]

    Marini, Andrea; Biancalana, Fabio

    2014-01-01T23:59:59.000Z

    We theoretically propose and investigate an optical analogue of neutrino oscillations in a pair of vertically displaced binary waveguide arrays with longitudinally modulated effective refractive index. Optical propagation is modelled through coupled-mode equations, which in the continuous limit lead to two coupled Dirac equations for fermionic particles with different mass states, i.e. neutrinos. We demonstrate that neutrino oscillations can be quenched by nonlinear effects, and we predict the existence of neutrino solitons. Incidentally, these phenomena are expected to play an important role in massive supernova stars. Our results pave the way for using binary waveguide arrays as a classical laboratory for predicting exotic effects in particle physics and astrophysics.

  17. Optical simulation of neutrino oscillations in binary waveguide arrays

    E-Print Network [OSTI]

    Andrea Marini; Stefano Longhi; Fabio Biancalana

    2014-05-06T23:59:59.000Z

    We theoretically propose and investigate an optical analogue of neutrino oscillations in a pair of vertically displaced binary waveguide arrays with longitudinally modulated effective refractive index. Optical propagation is modelled through coupled-mode equations, which in the continuous limit lead to two coupled Dirac equations for fermionic particles with different mass states, i.e. neutrinos. We demonstrate that neutrino oscillations can be quenched by nonlinear effects, and we predict the existence of neutrino solitons. Incidentally, these phenomena are expected to play an important role in massive supernova stars. Our results pave the way for using binary waveguide arrays as a classical laboratory for predicting exotic effects in particle physics and astrophysics.

  18. Some comments on the electrodynamics of binary pulsars

    E-Print Network [OSTI]

    Sobacchi, Emanuele

    2015-01-01T23:59:59.000Z

    We consider the electrodynamics of in-spiraling binary pulsars, showing that there are two distinct ways in which they may emit radiation. On the one hand, even if the pulsars do not rotate, we show that in vacuo orbital rotation generates magnetic quadrupole emission, which, in the late stages of the binary evolution becomes nearly as effective as magnetic dipole emission by a millisecond pulsar. On the other hand, we show that interactions of the two magnetic fields generate powerful induction electric fields, which cannot be screened by a suitable distribution of charges and currents like they are in isolated pulsars. We compute approximate electromotive forces for this case.

  19. Post common envelope binaries from SDSS. IV: SDSSJ121258.25-012310.1, a new eclipsing system

    E-Print Network [OSTI]

    Gómez-Morán, A Nebot; Schreiber, M R; Gänsicke, B T; Pyrzas, S; Schwarz, R; Southworth, J; Kohnert, J; Vogel, J; Krumpe, M; Rodríguez-Gil, P

    2009-01-01T23:59:59.000Z

    From optical photometry we show that SDSSJ121258.25-012310.1 is a new eclipsing, post common-envelope binary with an orbital period of 8.06 hours and an eclipse length of 23 minutes. We observed the object over 11 nights in different bands and determined the ephemeris of the eclipse to HJD_mid = 2454104. 7086(2) + 0.3358706(5) x E, where numbers in parenthesis indicate the uncertainties in the last digit. The depth of the eclipse is 2.85 +/- 0.17 mag in the V band, 1.82 +/- 0.08 mag in the R band and 0.52 +/- 0.02 mag in the I band. From spectroscopic observations we measured the semi-amplitude of the radial velocity K_2 = 181 +/- 3 km/s for the secondary star. The stellar and binary parameters of the system were constrained from a) fitting the SDSS composite spectrum of the binary, b) using a K-band luminosty-mass relation for the secondary star, and c) from detailed analyses of the eclipse light curve. The white dwarf has an effective temperature of 17700 +/- 300 K, and its surface gravity is logg =7.53 +/-...

  20. Symmetric chains, Gelfand-Tsetlin chains, and the Terwilliger algebra of the binary Hamming scheme

    E-Print Network [OSTI]

    Srinivasan, Murali K.

    Symmetric chains, Gelfand-Tsetlin chains, and the Terwilliger algebra of the binary Hamming scheme of the Terwilliger algebra of the binary Hamming scheme. We also give a representation theoretic characterization constructive proof of the explicit block diagonalization of the Terwilliger algebra of the binary Hamming

  1. The concrete theory of numbers: initial numbers and wonderful properties of numbers repunit

    E-Print Network [OSTI]

    Boris V. Tarasov

    2007-04-07T23:59:59.000Z

    In this work initial numbers and repunit numbers have been studied. All numbers have been considered in a decimal notation. The problem of simplicity of initial numbers has been studied. Interesting properties of numbers repunit are proved: $gcd(R_a, R_b) = R_{gcd(a,b)}$; $R_{ab}/(R_aR_b)$ is an integer only if $gcd(a,b) = 1$, where $a\\geq1$, $b\\geq1$ are integers. Dividers of numbers repunit, are researched by a degree of prime number.

  2. Production and Injection data for NV Binary facilities

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Mines, Greg

    Excel files are provided with well production and injection data for binary facilities in Nevada. The files contain the data that reported montly to the Nevada Bureau of Mines and Geology (NBMG) by the facility operators. this data has been complied into Excel spreadsheets for each of the facilities given on the NBMG web site.

  3. Production and Injection data for NV Binary facilities

    SciTech Connect (OSTI)

    Mines, Greg

    2013-12-24T23:59:59.000Z

    Excel files are provided with well production and injection data for binary facilities in Nevada. The files contain the data that reported montly to the Nevada Bureau of Mines and Geology (NBMG) by the facility operators. this data has been complied into Excel spreadsheets for each of the facilities given on the NBMG web site.

  4. Synthesis and characterization of nanocrystalline binary and ternary intermetallic compounds 

    E-Print Network [OSTI]

    Leonard, Brian Matthew

    2009-05-15T23:59:59.000Z

    nanocrystalline powders. Using this process, I was able to access several binary and ternary intermetallics, including two new phases: AuCuSn2 and AuNiSn2. These compounds were isolated as nanocrystals using low temperature solution synthesis techniques, which had...

  5. Accumulate-Repeat-Accumulate Codes: Systematic Codes Achieving the Binary

    E-Print Network [OSTI]

    Sason, Igal

    Accumulate-Repeat-Accumulate Codes: Systematic Codes Achieving the Binary Erasure Channel Capacity@ee.technion.ac.il Abstract The paper introduces ensembles of accumulate-repeat-accumulate (ARA) codes which asymp- totically by the first capacity-achieving ensembles of ir- regular repeat-accumulate (IRA) codes with bounded complexity

  6. Binary and recycled pulsars: 30 years after observational discovery

    E-Print Network [OSTI]

    G S Bisnovatyi-Kogan

    2006-11-13T23:59:59.000Z

    Binary radio pulsars, first discovered by Hulse and Taylor in 1974 [1], are a unique tool for experimentally testing general relativity (GR), whose validity has been confirmed with a precision unavailable in laboratory experiments. In particular, indirect evidence of the existence of gravitational waves has been obtained. Radio pulsars in binary systems (which have come to be known as recycled) have completed the accretion stage, during which neutron star spins reach millisecond periods and their magnetic fields decay 2 to 4 orders of magnitude more weakly than ordinary radio pulsars. Among about a hundred known recycled pulsars, many have turned out to be single neutron stars. The high concentration of single recycled pulsars in globular clusters suggests that close stellar encounters are highly instrumental in the loss of the companion. A system of one recycled pulsar and one 'normal' one discovered in 2004 is the most compact among binaries containing recycled pulsars [2]. Together with the presence of two pulsars in one system, this suggests new prospects for further essential improvements in testing GR. This paper considers theoretical predictions of binary pulsars, their evolutionary formation, and mechanisms by which their companions may be lost. The use of recycled pulsars in testing GR is discussed and their possible relation to the most intriguing objects in the universe, cosmic gamma-ray bursts, is examined.

  7. Coal liquefaction process using pretreatment with a binary solvent mixture

    DOE Patents [OSTI]

    Miller, Robert N. (Allentown, PA)

    1986-01-01T23:59:59.000Z

    An improved process for thermal solvent refining or hydroliquefaction of non-anthracitic coal at elevated temperatures under hydrogen pressure in a hydrogen donor solvent comprises pretreating the coal with a binary mixture of an aromatic hydrocarbon and an aliphatic alcohol at a temperature below 300.degree. C. before the hydroliquefaction step. This treatment generally increases both conversion of coal and yields of oil.

  8. Detecting gravitational waves from highly eccentric compact binaries

    E-Print Network [OSTI]

    Kai Sheng Tai; Sean T. McWilliams; Frans Pretorius

    2014-03-30T23:59:59.000Z

    In dense stellar regions, highly eccentric binaries of black holes and neutron stars can form through various n-body interactions. Such a binary could emit a significant fraction of its binding energy in a sequence of largely isolated gravitational wave bursts prior to merger. Given expected black hole and neutron star masses, many such systems will emit these repeated bursts at frequencies within the sensitive band of contemporary ground-based gravitational wave detectors. Unfortunately, existing gravitational wave searches are ill-suited to detect these signals. In this work, we adapt a "power stacking" method to the detection of gravitational wave signals from highly eccentric binaries. We implement this method as an extension of the Q-transform, a projection onto a multiresolution basis of windowed complex exponentials that has previously been used to analyze data from the network of LIGO/Virgo detectors. Our method searches for excess power over an ensemble of time-frequency tiles. We characterize the performance of our method using Monte Carlo experiments with signals injected in simulated detector noise. Our results indicate that the power stacking method achieves substantially better sensitivity to eccentric binary signals than existing localized burst searches.

  9. Dixie Valley Binary Cycle Production Data 2013 YTD

    SciTech Connect (OSTI)

    Lee, Vitaly

    2013-10-18T23:59:59.000Z

    Proving the technical and economic feasibility of utilizing the available unused heat to generate additional electric power from a binary power plant from the low-temperature brine at the Dixie Valley Geothermal Power Plant. Monthly data for Jan 2013-September 2013

  10. Robust Target Localization from Binary Decisions in Wireless Sensor Networks

    E-Print Network [OSTI]

    Michailidis, George

    Robust Target Localization from Binary Decisions in Wireless Sensor Networks Natallia Katenka Wireless sensor networks (WSN) are becoming an important tool in a variety of tasks, including mon- itoring targets and localizing multiple targets are also considered. Keywords: wireless sensor network, target

  11. Every interacting double white dwarf binary may merge

    E-Print Network [OSTI]

    Shen, Ken J

    2015-01-01T23:59:59.000Z

    Interacting double white dwarf binaries can give rise to a wide variety of astrophysical outcomes ranging from faint thermonuclear and Type Ia supernovae to the formation of neutron stars and stably accreting AM Canum Venaticorum systems. One key factor affecting the final outcome is whether mass transfer remains dynamically stable or instead diverges, leading to the tidal disruption of the donor and the merger of the binary. It is typically thought that for low ratios of the donor mass to the accretor mass, mass transfer remains stable, especially if accretion occurs via a disk. In this Letter, we examine disk-accreting binaries with extremely low mass ratios and find that the initial phase of hydrogen-rich mass transfer leads to a classical nova-like outburst on the accretor. Dynamical friction within the expanding nova shell shrinks the orbit and causes the mass transfer rate to increase dramatically above the accretor's Eddington limit, resulting in a binary merger. While further calculations are necessar...

  12. First-post-Newtonian quadrupole tidal interactions in binary systems

    E-Print Network [OSTI]

    Justin Vines; Éanna É. Flanagan

    2014-10-09T23:59:59.000Z

    We consider tidal coupling in a binary stellar system to first-post-Newtonian order. We derive the orbital equations of motion for bodies with spins and mass quadrupole moments and show that they conserve the total linear momentum of the binary. We note that spin-orbit coupling must be included in a 1PN treatment of tidal interactions in order to maintain consistency (except in the special case of adiabatically induced quadrupoles); inclusion of 1PN quadrupolar tidal effects while omitting spin effects would lead to a failure of momentum conservation for generic evolution of the quadrupoles. We use momentum conservation to specialize our analysis to the system's center-of-mass-energy frame; we find the binary's relative equation of motion in this frame and also present a generalized Lagrangian from which it can be derived. We then specialize to the case in which the quadrupole moment is adiabatically induced by the tidal field (in which case it is consistent to ignore spin effects). We show how the adiabatic dynamics for the quadrupole can be incorporated into our action principle and present the simplified orbital equations of motion and conserved energy for the adiabatic case. These results are relevant to gravitational wave signals from inspiralling binary neutron stars.

  13. A detection pipeline for galactic binaries in LISA data

    E-Print Network [OSTI]

    Tyson B. Littenberg

    2011-06-30T23:59:59.000Z

    The Galaxy is suspected to contain hundreds of millions of binary white dwarf systems, a large fraction of which will have sufficiently small orbital period to emit gravitational radiation in band for space-based gravitational wave detectors such as the Laser Interferometer Space Antenna (LISA). LISA's main science goal is the detection of cosmological events (supermassive black hole mergers, etc.) however the gravitational signal from the galaxy will be the dominant contribution to the data -- including instrumental noise -- over approximately two decades in frequency. The catalogue of detectable binary systems will serve as an unparalleled means of studying the Galaxy. Furthermore, to maximize the scientific return from the mission, the data must be "cleansed" of the galactic foreground. We will present an algorithm that can accurately resolve and subtract >10000 of these sources from simulated data supplied by the Mock LISA Data Challenge Task Force. Using the time evolution of the gravitational wave frequency, we will reconstruct the position of the recovered binaries and show how LISA will sample the entire compact binary population in the Galaxy.

  14. Reliable Computation of Binary Parameters in Activity Coefficient Models

    E-Print Network [OSTI]

    Stadtherr, Mark A.

    phase equilibria. The technique is demonstrated with examples using the NRTL and electrolyte-NRTL (eNRTL) models. In two of the NRTL examples, results are found that contradict previous work. In the eNRTL time that a method for parameter estimation in the eNRTL model from binary LLE data (mutual solubility

  15. A New Merging Double Degenerate Binary in the Solar Neighborhood

    E-Print Network [OSTI]

    Debes, John H; Tremblay, Pier-Emmanuel; López-Morales, Mercedes; Anglada-Escudé, Guillem; Napiwotzki, Ralf; Osip, David; Weinberger, Alycia

    2015-01-01T23:59:59.000Z

    Characterizing the local space density of double degenerate binary systems is a complementary approach to broad sky surveys of double degenerates to determine the expected rates of white dwarf binary mergers, in particular those that may evolve into other observable phenomena such as extreme helium stars, Am CVn systems, and supernovae Ia. However, there have been few such systems detected in local space. We report here the discovery that WD 1242$-$105, a nearby bright WD, is a double-line spectroscopic binary consisting of two degenerate DA white dwarfs of similar mass and temperature, despite it previously having been spectroscopically characterized as a single degenerate. Follow-up photometry, spectroscopy, and trigonometric parallax have been obtained in an effort to determine the fundamental parameters of each component of this system. The binary has a mass ratio of 0.7 and a trigonometric parallax of 25.5 mas, placing it at a distance of 39 pc. The system's total mass is 0.95 M$_\\odot$ and has an orbita...

  16. Binary recycled pulsars, as a most precise physical laboratory

    E-Print Network [OSTI]

    G. S. Bisnovatyi-Kogan

    2008-02-08T23:59:59.000Z

    The following problems are discussed. 1. Pulsars and close binaries. 2. Hulse-Taylor pulsar. 3. Disrupted pulsar pairs. 4. RP statistics. 5. Enhanced evaporation: formation of single RP. 6. General relativity effects: NS+NS. 7. A Double pulsar system. 8. Checking general relativity. 9. Variability of the gravitational constant. 10. Space Watch.

  17. DIRECT N-BODY MODELING OF THE OLD OPEN CLUSTER NGC 188: A DETAILED COMPARISON OF THEORETICAL AND OBSERVED BINARY STAR AND BLUE STRAGGLER POPULATIONS

    SciTech Connect (OSTI)

    Geller, Aaron M. [Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208 (United States); Hurley, Jarrod R. [Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122 (Australia); Mathieu, Robert D., E-mail: a-geller@northwestern.edu, E-mail: mathieu@astro.wisc.edu, E-mail: jhurley@astro.swin.edu.au [Department of Astronomy, University of Wisconsin-Madison, Madison, WI 53706 (United States)

    2013-01-01T23:59:59.000Z

    Following on from a recently completed radial-velocity survey of the old (7 Gyr) open cluster NGC 188 in which we studied in detail the solar-type hard binaries and blue stragglers of the cluster, here we investigate the dynamical evolution of NGC 188 through a sophisticated N-body model. Importantly, we employ the observed binary properties of the young (180 Myr) open cluster M35, where possible, to guide our choices for parameters of the initial binary population. We apply pre-main-sequence tidal circularization and a substantial increase to the main-sequence tidal circularization rate, both of which are necessary to match the observed tidal circularization periods in the literature, including that of NGC 188. At 7 Gyr the main-sequence solar-type hard-binary population in the model matches that of NGC 188 in both binary frequency and distributions of orbital parameters. This agreement between the model and observations is in a large part due to the similarities between the NGC 188 and M35 solar-type binaries. Indeed, among the 7 Gyr main-sequence binaries in the model, only those with P {approx}> 1000 days begin to show potentially observable evidence for modifications by dynamical encounters, even after 7 Gyr of evolution within the star cluster. This emphasizes the importance of defining accurate initial conditions for star cluster models, which we propose is best accomplished through comparisons with observations of young open clusters like M35. Furthermore, this finding suggests that observations of the present-day binaries in even old open clusters can provide valuable information on their primordial binary populations. However, despite the model's success at matching the observed solar-type main-sequence population, the model underproduces blue stragglers and produces an overabundance of long-period circular main-sequence-white-dwarf binaries as compared with the true cluster. We explore several potential solutions to the paucity of blue stragglers and conclude that the model dramatically underproduces blue stragglers through mass-transfer processes. We suggest that common-envelope evolution may have been incorrectly imposed on the progenitors of the spurious long-period circular main-sequence-white-dwarf binaries, which perhaps instead should have gone through stable mass transfer to create blue stragglers, thereby bringing both the number and binary frequency of the blue straggler population in the model into agreement with the true blue stragglers in NGC 188. Thus, improvements in the physics of mass transfer and common-envelope evolution employed in the model may in fact solve both discrepancies with the observations. This project highlights the unique accessibility of open clusters to both comprehensive observational surveys and full-scale N-body simulations, both of which have only recently matured sufficiently to enable such a project, and underscores the importance of open clusters to the study of star cluster dynamics.

  18. A new detached K7 dwarf eclipsing binary system

    E-Print Network [OSTI]

    T. B. Young; M. G. Hidas; J. K. Webb; M. C. B. Ashley; J. L. Christiansen; A. Derekas; C. Nutto

    2007-03-22T23:59:59.000Z

    We present an analysis of a new, detached, double-lined eclipsing binary system with K7 Ve components, discovered as part of the University of New South Wales Extrasolar Planet Search. The object is significant in that only 6 other binary systems are known with comparable or lower mass. Such systems offer important tests of mass-radius theoretical models. Follow-up photometry and spectroscopy were obtained with the 40-inch and 2.3m telescopes at SSO respectively. An estimate of the radial velocity amplitude from spectral absorption features, combined with the orbital inclination (83.5 deg) estimated from lightcurve fitting, yielded a total mass of M=(1.041 +/- 0.06)M_sun and component masses of M_A=(0.529 +/- 0.035)M_sun and M_B=(0.512 +/- 0.035)M_sun. The radial velocity amplitude estimated from absorption features (167 +/- 3)kmps was found to be less than the estimate from the H_alpha emission lines (175 +/- 1.5)kmps. The lightcurve fit produced radii of R_A=(0.641 +/- 0.05)R_sun and R_B=(0.608 +/- 0.06)R_sun, and a temperature ratio of T_B/T_A=0.980 +/- 0.015. The apparent magnitude of the binary was estimated to be V=13.9 +/- 0.2. Combined with the spectral type, this gave the distance to the binary as 169 +/- 14 pc. The timing of the secondary eclipse gave a lower limit on the eccentricity of the binary system of 0.0025 +/- 0.0005. This is the most statistically significant non-zero eccentricity found for such a system, possibly suggesting the presence of a third companion.

  19. Resonant Oscillations and Tidal Heating in Coalescing Binary Neutron Stars

    E-Print Network [OSTI]

    Dong Lai

    1994-04-25T23:59:59.000Z

    Tidal interaction in a coalescing neutron star binary can resonantly excite the g-mode oscillations of the neutron star when the frequency of the tidal driving force equals the intrinsic g-mode frequencies. We study the g-mode oscillations of cold neutron stars using recent microscopic nuclear equations of state, where we determine self-consistently the sound speed and Brunt-V\\"ais\\"al\\"a frequency in the nuclear liquid core. The properties of the g-modes associated with the stable stratification of the core depend sensitively on the pressure-density relation as well as the symmetry energy of the dense nuclear matter. The frequencies of the first ten g-modes lie approximately in the range of $10-100$ Hz. Resonant excitations of these g-modes during the last few minutes of the binary coalescence result in energy transfer and angular momentum transfer from the binary orbit to the neutron star. The angular momentum transfer is possible because a dynamical tidal lag develops even in the absence of fluid viscosity. However, since the coupling between the g-mode and the tidal potential is rather weak, the amount of energy transfer during a resonance and the induced orbital phase error are very small. Resonant excitations of the g-modes play an important role in tidal heating of binary neutron stars. Without the resonances, viscous dissipation is effective only when the stars are close to contact. The resonant oscillations result in dissipation at much larger orbital separation. The actual amount of tidal heating depends on the viscosity of the neutron star. Using the microscopic viscosity, we find that the binary neutron stars are heated to a temperature $\\sim 10^8$ K before they come into contact.

  20. The contact binary GSC 04778-00152 with a visual companion

    E-Print Network [OSTI]

    T. Tuvikene; T. Eenmäe; C. Sterken; E. Brogt

    2008-09-11T23:59:59.000Z

    Photometric and spectroscopic observations of the unstudied 12th-magnitude eclipsing binary GSC 04778-00152 are presented. We report the discovery of a visual companion about 1 mag fainter and 2 arcsec away from the binary. By subtracting the light contribution of the visual companion, we obtain the UBVRI light curves of the binary system alone. The shape of the light curve indicates that GSC 04778-00152 is an A-type W UMa contact binary. From light-curve modeling, we derive parameters of the binary system.

  1. Efficiency of mass transfer in massive close binaries, Tests from double-lined eclipsing binaries in the SMC

    E-Print Network [OSTI]

    S. E. de Mink; O. R. Pols; R. W. Hilditch

    2007-03-19T23:59:59.000Z

    One of the major uncertainties in close binary evolution is the efficiency of mass transfer beta: the fraction of transferred mass that is accreted by a secondary star. We attempt to constrain the mass-transfer efficiency for short-period massive binaries undergoing case A mass transfer. We present a grid of about 20,000 detailed binary evolution tracks with primary masses 3.5-35 Msun, orbital periods 1-5 days at a metallicity Z=0.004, assuming both conservative and non-conservative mass transfer. We perform a systematic comparison, using least-squares fitting, of the computed models with a sample of 50 double-lined eclipsing binaries in the Small Magellanic Cloud, for which fundamental stellar parameters have been determined. About 60% of the systems are currently undergoing slow mass transfer. In general we find good agreement between our models and the observed detached systems. However, for many of the semi-detached systems the observed temperature ratio is more extreme than our models predict. For the 17 semi-detached systems that we are able to match, we find a large spread in the best fitting mass-transfer efficiency; no single value of beta can explain all systems. We find a hint that initially wider systems tend to fit better to less conservative models. We show the need for more accurate temperature determinations and we find that determinations of surface abundances of nitrogen and carbon can potentially constrain the mass-transfer efficiency further.

  2. KEPLER ECLIPSING BINARY STARS. III. CLASSIFICATION OF KEPLER ECLIPSING BINARY LIGHT CURVES WITH LOCALLY LINEAR EMBEDDING

    SciTech Connect (OSTI)

    Matijevic, Gal [Faculty of Mathematics and Physics, University of Ljubljana, Jadranska 19, 1000 Ljubljana (Slovenia); Prsa, Andrej [Department of Astronomy and Astrophysics, Villanova University, 800 E Lancaster Ave, Villanova, PA 19085 (United States); Orosz, Jerome A.; Welsh, William F. [Department of Astronomy, San Diego State University, 5500 Campanile Dr., San Diego, CA 92182 (United States); Bloemen, Steven [Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200 D, B-3001 Leuven (Belgium); Barclay, Thomas, E-mail: gal.matijevic@fmf.uni-lj.si, E-mail: andrej.prsa@villanova.edu [NASA Ames Research Center/BAER Institute, Moffett Field, CA 94035 (United States)

    2012-05-15T23:59:59.000Z

    We present an automated classification of 2165 Kepler eclipsing binary (EB) light curves that accompanied the second Kepler data release. The light curves are classified using locally linear embedding, a general nonlinear dimensionality reduction tool, into morphology types (detached, semi-detached, overcontact, ellipsoidal). The method, related to a more widely used principal component analysis, produces a lower-dimensional representation of the input data while preserving local geometry and, consequently, the similarity between neighboring data points. We use this property to reduce the dimensionality in a series of steps to a one-dimensional manifold and classify light curves with a single parameter that is a measure of 'detachedness' of the system. This fully automated classification correlates well with the manual determination of morphology from the data release, and also efficiently highlights any misclassified objects. Once a lower-dimensional projection space is defined, the classification of additional light curves runs in a negligible time and the method can therefore be used as a fully automated classifier in pipeline structures. The classifier forms a tier of the Kepler EB pipeline that pre-processes light curves for the artificial intelligence based parameter estimator.

  3. Data Compression with Prime Numbers

    E-Print Network [OSTI]

    Gordon Chalmers

    2005-11-16T23:59:59.000Z

    A compression algorithm is presented that uses the set of prime numbers. Sequences of numbers are correlated with the prime numbers, and labeled with the integers. The algorithm can be iterated on data sets, generating factors of doubles on the compression.

  4. X-Ray Binary Systems in the Small Magellanic Cloud

    E-Print Network [OSTI]

    P. Kahabka; W. Pietsch

    1997-06-09T23:59:59.000Z

    We present the result of a systematic search for spectrally hard and soft X-ray binary systems in the Small Magellanic Cloud (SMC). This search has been applied to ROSAT PSPC data (0.1-2.4 keV) collected during 9 pointed observations towards this galaxy covering a time span of 2 years from October 91 till October 93. Selection criteria have been defined in order to confine the sample of candidates. Finally 7 spectrally hard and 4 spectrally soft sources were selected from the list as candidates for binaries in the SMC. The sample is luminosity limited (>3.10**35 erg/s). SMC X-1 has been observed during a full binary orbit starting with a low-state covering an X-ray eclipse and emerging into a bright long-duration flare with two short-duration flares separated by 10 hours. The Be type transient SMC X-2 has been redetected with ROSAT. Variability has been found in the sources RX J0051.8-7231 and RX J0052.1-731 already discovered with Einstein. RX J0101.0-7206 has been discovered at the north-eastern boundary of the giant SMC HII region N66 during an X-ray outburst and half a year later during a quiescent phase. A variable source, RX J0049.1-7250, located north-east of the SMC supernova remnant N19 and which may either be an X-ray binary or an AGN turns out to be strongly absorbed. It may be located behind the SMC. If it is an X-ray binary then it radiates at the Eddington limit in the X-ray bright state. Another variable and hard X-ray source RX J0032.9-7348 has been discovered at the south-eastern border of the body of the SMC. A high mass X-ray binary nature is favored for this source. We searched for CAL87 like systems in the SMC catalog and found none. A new candidate supersoft source RX J0103.8-7254 has been detected. We cannot exclude that it is a foreground object.

  5. Accretion Disc Evolution in Single and Binary T Tauri Stars

    E-Print Network [OSTI]

    Philip J. Armitage; C. J. Clarke; C. A. Tout

    1998-10-30T23:59:59.000Z

    We present theoretical models for the evolution of T Tauri stars surrounded by circumstellar discs. The models include the effects of pre-main-sequence stellar and time dependent disc evolution, and incorporate the effects of stellar magnetic fields acting on the inner disc. For single stars, consistency with observations in Taurus-Auriga demands that disc dispersal occurs rapidly, on much less than the viscous timescale of the disc, at roughly the epoch when heating by stellar radiation first dominates over internal viscous dissipation. Applying the models to close binaries, we find that because the initial conditions for discs in binaries are uncertain, studies of extreme mass ratio systems are required to provide a stringent test of theoretical disc evolution models. We also note that no correlation of the infra-red colours of T Tauri stars with their rotation rate is observed, in apparent contradiction to the predictions of simple magnetospheric accretion models.

  6. General Relativistic Binary Merger Simulations and Short Gamma Ray Bursts

    E-Print Network [OSTI]

    Joshua A. Faber; Thomas W. Baumgarte; Stuart L. Shapiro; Keisuke Taniguchi

    2006-03-10T23:59:59.000Z

    The recent localization of some short-hard gamma ray bursts (GRBs) in galaxies with low star formation rates has lent support to the suggestion that these events result from compact object binary mergers. We discuss how new simulations in general relativity are helping to identify the central engine of short-hard GRBs. Motivated by our latest relativistic black hole-neutron star merger calculations, we discuss a scenario in which these events may trigger short-hard GRBs, and compare this model to competing relativistic models involving binary neutron star mergers and the delayed collapse of hypermassive neutron stars. Distinguishing features of these models may help guide future GRB and gravitational wave observations to identify the nature of the sources.

  7. Planet formation around binary stars: Tatooine made easy

    E-Print Network [OSTI]

    Bromley, B C

    2015-01-01T23:59:59.000Z

    We examine characteristics of circumbinary orbits in the context of current planet formation scenarios. Analytical perturbation theory predicts the existence of nested circumbinary orbits that are generalizations of circular orbits in a Keplerian potential. They contain forced epicyclic motion aligned with the binary as well as higher frequency oscillations, yet they do not cross, even in the presence of massive disks and perturbations from large planets. For this reason, dissipative gas and planetesimals can settle onto these "most circular" orbits, facilitating the growth of protoplanets. Outside a region close to the binary where orbits are generally unstable, circumbinary planets form in much the same way as their cousins around a single star. Here, we review the theory and confirm its predictions with a suite of representative simulations. We then consider the circumbinary planets discovered with NASA's Kepler satellite. These Neptune- and Jupiter-size planets, or their planetesimal precursors, may have ...

  8. Simulations of binary black hole mergers using spectral methods

    SciTech Connect (OSTI)

    Szilagyi, Bela; Lindblom, Lee; Scheel, Mark A. [Theoretical Astrophysics 350-17, California Institute of Technology, Pasadena, California 91125 (United States)

    2009-12-15T23:59:59.000Z

    Several improvements in numerical methods and gauge choice are presented that make it possible now to perform simulations of the merger and ringdown phases of 'generic' binary black hole evolutions using the pseudospectral evolution code SpEC. These improvements include the use of a new damped-wave gauge condition, a new grid structure with appropriate filtering that improves stability, and better adaptivity in conforming the grid structures to the shapes and sizes of the black holes. Simulations illustrating the success of these new methods are presented for a variety of binary black hole systems. These include fairly generic systems with unequal masses (up to 2 ratio 1 mass ratios), and spins (with magnitudes up to 0.4M{sup 2}) pointing in various directions.

  9. Kinetic Theory for Binary Granular Mixtures at Low-Density

    E-Print Network [OSTI]

    Vicente Garzo

    2007-04-10T23:59:59.000Z

    Many features of granular media can be modelled as a fluid of hard spheres with {\\em inelastic} collisions. Under rapid flow conditions, the macroscopic behavior of grains can be described through hydrodynamic equations. At low-density, a fundamental basis for the derivation of the hydrodynamic equations and explicit expressions for the transport coefficients appearing in them is provided by the Boltzmann kinetic theory conveniently modified to account for inelastic binary collisions. The goal of this chapter is to give an overview of the recent advances made for binary granular gases by using kinetic theory tools. Some of the results presented here cover aspects such as transport properties, energy nonequipartition, instabilities, segregation or mixing, non-Newtonian behavior, .... In addition, comparison of the analytical results with those obtained from Monte Carlo and molecular dynamics simulations is also carried out, showing the reliability of kinetic theory to describe granular flows even for strong dissipation.

  10. Development of a Physiologically Based Pharmacokinetic and Pharmacodynamic Model to Determine Dosimetry and Cholinesterase Inhibition for a Binary Mixture of Chlorpyrifos and Diazinon in the Rat

    SciTech Connect (OSTI)

    Timchalk, Chuck; Poet, Torka S.

    2008-05-01T23:59:59.000Z

    Physiologically based pharmacokinetic/pharmacodynamic (PBPK/PD) models have been developed and validated for the organophosphorus (OP) insecticides chlorpyrifos (CPF) and diazinon (DZN). Based on similar pharmacokinetic and mode of action properties it is anticipated that these OPs could interact at a number of important metabolic steps including: CYP450 mediated activation/detoxification, and blood/tissue cholinesterase (ChE) binding/inhibition. We developed a binary PBPK/PD model for CPF, DZN and their metabolites based on previously published models for the individual insecticides. The metabolic interactions (CYP450) between CPF and DZN were evaluated in vitro and suggests that CPF is more substantially metabolized to its oxon metabolite than is DZN. These data are consistent with their observed in vivo relative potency (CPF>DZN). Each insecticide inhibited the other’s in vitro metabolism in a concentration-dependent manner. The PBPK model code used to described the metabolism of CPF and DZN was modified to reflect the type of inhibition kinetics (i.e. competitive vs. non-competitive). The binary model was then evaluated against previously published rodent dosimetry and ChE inhibition data for the mixture. The PBPK/PD model simulations of the acute oral exposure to single- (15 mg/kg) vs. binary-mixtures (15+15 mg/kg) of CFP and DZN at this lower dose resulted in no differences in the predicted pharmacokinetics of either the parent OPs or their respective metabolites; whereas, a binary oral dose of CPF+DZN at 60+60 mg/kg did result in observable changes in the DZN pharmacokinetics. Cmax was more reasonably fit by modifying the absorption parameters. It is anticipated that at low environmentally relevant binary doses, most likely to be encountered in occupational or environmental related exposures, that the pharmacokinetics are expected to be linear, and ChE inhibition dose-additive.

  11. A fractal set from the binary reflected Gray code

    E-Print Network [OSTI]

    J. A. Oteo; J. Ros

    2005-10-14T23:59:59.000Z

    The permutation associated with the decimal expression of the binary reflected Gray code with $N$ bits is considered. Its cycle structure is studied. Considered as a set of points, its self-similarity is pointed out. As a fractal, it is shown to be the attractor of a IFS. For large values of $N$ the set is examined from the point of view of time series analysis

  12. Coal liquefaction process using pretreatment with a binary solvent mixture

    DOE Patents [OSTI]

    Miller, R.N.

    1986-10-14T23:59:59.000Z

    An improved process for thermal solvent refining or hydroliquefaction of non-anthracitic coal at elevated temperatures under hydrogen pressure in a hydrogen donor solvent comprises pretreating the coal with a binary mixture of an aromatic hydrocarbon and an aliphatic alcohol at a temperature below 300 C before the hydroliquefaction step. This treatment generally increases both conversion of coal and yields of oil. 1 fig.

  13. Linear Complexity Lossy Compressor for Binary Redundant Memoryless Sources

    E-Print Network [OSTI]

    Mimura, Kazushi

    2011-01-01T23:59:59.000Z

    A lossy compression algorithm for binary redundant i.i.d. sources is presented. The proposed scheme is based on sparse graph codes. By introducing a nonlinear function, redundant memoryless sequences can be compressed. We propose a linear complexity compressor based on the extended belief propagation, into which an inertia term is heuristically introduced, and show that it has near optimal performance for moderate blocklengths.

  14. Gravitational-wave modes from precessing black-hole binaries

    E-Print Network [OSTI]

    Michael Boyle; Lawrence E. Kidder; Serguei Ossokine; Harald P. Pfeiffer

    2014-09-22T23:59:59.000Z

    Gravitational waves from precessing black-hole binaries exhibit features that are absent in nonprecessing systems. The most prominent of these is a parity-violating asymmetry that beams energy and linear momentum preferentially along or opposite to the orbital angular momentum, leading to recoil of the binary. The asymmetry will appear as amplitude and phase modulations at the orbital frequency. For strongly precessing systems, it accounts for at least 3% amplitude modulation for binaries in the sensitivity band of ground-based gravitational-wave detectors, and can exceed 50% for massive systems. Such asymmetric features are also clearly visible when the waves are decomposed into modes of spin-weighted spherical harmonics, and are inherent in the waves themselves---rather than resulting from residual eccentricity in numerical simulations, or from mode-mixing due to precession. In particular, there is generically no instantaneous frame for which the mode decomposition will have any symmetry. We introduce a method to simplify the expressions for waveforms given in analytical relativity, which can be used to combine existing high-order waveforms for nonprecessing systems with expressions for the precessing contributions, leading to improved accuracy and a unified treatment of precessing and nonprecessing binaries. Using this method, it is possible to clarify the nature and the origins of the asymmetries and show the effects of asymmetry on recoils more clearly. We present post-Newtonian (PN) expressions for the waveform modes that include these terms, complete to the relative 2PN level in spin (proportional to $v^4/c^4$ times a certain combination of the spins). Comparing the results of those expressions to numerical results, we find good qualitative agreement. We also demonstrate how these expressions can be used to efficiently calculate waveforms for gravitational-wave astronomy.

  15. Short Gamma-Ray Bursts from Binary Neutron Star Mergers

    E-Print Network [OSTI]

    Roland Oechslin; Thomas Janka

    2006-04-27T23:59:59.000Z

    We present the results from new relativistic hydrodynamic simulations of binary neutron star mergers using realistic non-zero temperature equations of state. We vary several unknown parameters in the system such as the neutron star (NS) masses, their spins and the nuclear equation of state. The results are then investigated with special focus on the post-merger torus-remnant system. Observational implications on the Gamma-ray burst (GRB) energetics are discussed and compared with recent observations.

  16. A study of diffusion in binary solutions using spin echoes 

    E-Print Network [OSTI]

    Rousseau, Cecil Clyde

    1962-01-01T23:59:59.000Z

    of Experimentally Determined Diffusion Coefficients of Cyclohexane and Acetone with the Results of NcCall, Douglass, and Anderson . . . . . . . . . 23 INTRODUCTION The available descriptions of the liquid state form a continuous spectrum that extends from... the liquid with unit velocity. The intrinsic diffusion coefficient is now given by Di kT Equation (1-11) is known as the Einstein relation. Thus far, no explicit statement has been made concerning diffusion in binary systems. In addition to the intrinsic...

  17. DUST GRAIN EVOLUTION IN SPATIALLY RESOLVED T TAURI BINARIES

    SciTech Connect (OSTI)

    Skemer, Andrew J.; Close, Laird M.; Hinz, Philip M.; Hoffmann, William F.; Males, Jared R. [Steward Observatory, Department of Astronomy, University of Arizona, Tucson, AZ 85721 (United States); Greene, Thomas P. [NASA Ames Research Center, Moffett Field, CA 94035 (United States)

    2011-10-10T23:59:59.000Z

    Core-accretion planet formation begins in protoplanetary disks with the growth of small, interstellar medium dust grains into larger particles. The progress of grain growth, which can be quantified using 10 {mu}m silicate spectroscopy, has broad implications for the final products of planet formation. Previous studies have attempted to correlate stellar and disk properties with the 10 {mu}m silicate feature in an effort to determine which stars are efficient at grain growth. Thus far there does not appear to be a dominant correlated parameter. In this paper, we use spatially resolved adaptive optics spectroscopy of nine T Tauri binaries as tight as 0.''25 to determine if basic properties shared between binary stars, such as age, composition, and formation history, have an effect on dust grain evolution. We find with 90%-95% confidence that the silicate feature equivalent widths of binaries are more similar than those of randomly paired single stars, implying that shared properties do play an important role in dust grain evolution. At lower statistical significance, we find with 82% confidence that the secondary has a more prominent silicate emission feature (i.e., smaller grains) than the primary. If confirmed by larger surveys, this would imply that spectral type and/or binarity are important factors in dust grain evolution.

  18. Resonant oscillations and tidal heating in coalescing binary neutron stars

    E-Print Network [OSTI]

    Lai, D

    1994-01-01T23:59:59.000Z

    Tidal interaction in a coalescing neutron star binary can resonantly excite the g-mode oscillations of the neutron star when the frequency of the tidal driving force equals the intrinsic g-mode frequencies. We study the g-mode oscillations of cold neutron stars using recent microscopic nuclear equations of state, where we determine self-consistently the sound speed and Brunt-V\\"ais\\"al\\"a frequency in the nuclear liquid core. The properties of the g-modes associated with the stable stratification of the core depend sensitively on the pressure-density relation as well as the symmetry energy of the dense nuclear matter. The frequencies of the first ten g-modes lie approximately in the range of 10-100 Hz. Resonant excitations of these g-modes during the last few minutes of the binary coalescence result in energy transfer and angular momentum transfer from the binary orbit to the neutron star. The angular momentum transfer is possible because a dynamical tidal lag develops even in the absence of fluid viscosity. ...

  19. The first pre-supersoft X-ray binary

    E-Print Network [OSTI]

    Parsons, S G; Gansicke, B T; Rebassa-Mansergas, A; Brahm, R; Zorotovic, M; Toloza, O; Pala, A F; Tappert, C; Bayo, A; Jordan, A

    2015-01-01T23:59:59.000Z

    We report the discovery of an extremely close white dwarf plus F dwarf main-sequence star in a 12 hour binary identified by combining data from the RAdial Velocity Experiment (RAVE) survey and the Galaxy Evolution Explorer (GALEX) survey. A combination of spectral energy distribution fitting and optical and Hubble Space Telescope ultraviolet spectroscopy allowed us to place fairly precise constraints on the physical parameters of the binary. The system, TYC 6760-497-1, consists of a hot Teff~21,500K, M~0.65Ms white dwarf and an F8 star (M~1.23Ms, R~1.35Rs) seen at a low inclination (i~35 deg). The system is likely the descendent of a binary that contained the F star and a ~2Ms A-type star that filled its Roche-lobe on the second asymptotic giant branch, initiating a common envelope phase. The F star is extremely close to Roche-lobe filling and there is likely to be a short phase of thermal timescale mass-transfer onto the white dwarf. During this phase it will grow in mass by up to 20 per cent, until the mass...

  20. PPl 15: The First Brown Dwarf Spectroscopic Binary

    E-Print Network [OSTI]

    Gibor Basri; Eduardo Martin

    1999-08-02T23:59:59.000Z

    PPl 15 is the first object to have been confirmed as a brown dwarf by the lithium test (in 1995), though its inferred mass was very close to the substellar limit. It is a member of the Pleiades open cluster. Its position in a cluster color-magnitude diagram suggested that it might be binary, and preliminary indications that it is a double-lined spectroscopic binary were reported by us in 1997. Here we report on the results of a consecutive week of Keck HIRES observations of this system, which yield its orbit. It has a period of about 5.8 days, and an eccentricity of 0.4+/-0.05. The rotation of the stars is slow for this class of objects. Because the system luminosity is divided between 2 objects with a mass ratio of 0.85, this renders each of them an incontrovertible brown dwarf, with masses between 60-70 jupiters. We show that component B is a little redder than A by studying their wavelength-dependent line ratios, and that this variation is compatible with the mass ratio. We confirm that the system has lithium, but cannot support the original conclusion that it is depleted (which would be surprising, given the new masses). This is a system of very close objects which, if they had combined, would have produced a low mass star. We discuss the implications of this discovery for the theories of binary formation and formation of very low mass objects.

  1. A Lossless Fuzzy Binary AND/OR Compressor

    E-Print Network [OSTI]

    Alipour, Philip B

    2009-01-01T23:59:59.000Z

    In this report, a new fuzzy 2bit-AND parallel-to-OR, or simply, a fuzzy binary AND/OR (FBAR) text data compression model as an algorithm is suggested for bettering spatial locality limits on nodes during database transactions. The current model incorporates a four-layer application technique: string-to-AND/OR pairwise binary bit + fuzzy quantum with noise conversions. This technique promotes a lossless data compression ratio of 2:1 up to values approximately = 3:1, generating a spatially-efficient compressed data file compared to nowadays data compressors. Data decompression/specific data reconstruction initiates an AND/OR pattern match technique in respect of fuzzy quantum indicators in the binary function field. The reconstruction of data occurs in the 4th layer using encryption methods. It is hypothesized that significant data compression ratio of 2n:1 for n>3:1 ratios, e.g., 32~64:1 are achievable via fuzzy qubit indexing over classical byte blocks for every bit position fragmented into a (1/2 upper +1/2 ...

  2. Improved methods for simulating nearly extremal binary black holes

    E-Print Network [OSTI]

    Mark A. Scheel; Matthew Giesler; Daniel A. Hemberger; Geoffrey Lovelace; Kevin Kuper; Michael Boyle; Bela Szilagyi; Lawrence E. Kidder

    2014-12-04T23:59:59.000Z

    Astrophysical black holes could be nearly extremal (that is, rotating nearly as fast as possible); therefore, nearly extremal black holes could be among the binaries that current and future gravitational-wave observatories will detect. Predicting the gravitational waves emitted by merging black holes requires numerical-relativity simulations, but these simulations are especially challenging when one or both holes have mass $m$ and spin $S$ exceeding the Bowen-York limit of $S/m^2=0.93$. We present improved methods that enable us to simulate merging, nearly extremal black holes more robustly and more efficiently. We use these methods to simulate an unequal-mass, precessing binary black hole coalescence, where the larger black hole has $S/m^2=0.99$. We also use these methods to simulate a non-precessing binary black hole coalescence, where both black holes have $S/m^2=0.994$, nearly reaching the Novikov-Thorne upper bound for holes spun up by thin accretion disks. We demonstrate numerical convergence and estimate the numerical errors of the waveforms; we compare numerical waveforms from our simulations with post-Newtonian and effective-one-body waveforms; we compare the evolution of the black-hole masses and spins with analytic predictions; and we explore the effect of increasing spin magnitude on the orbital dynamics (the so-called "orbital hangup" effect).

  3. Simulating merging binary black holes with nearly extremal spins

    SciTech Connect (OSTI)

    Lovelace, Geoffrey [Center for Radiophysics and Space Research, Cornell University, Ithaca, New York, 14853 (United States); Scheel, Mark A.; Szilagyi, Bela [Theoretical Astrophysics 350-17, California Institute of Technology, Pasadena, California 91125 (United States)

    2011-01-15T23:59:59.000Z

    Astrophysically realistic black holes may have spins that are nearly extremal (i.e., close to 1 in dimensionless units). Numerical simulations of binary black holes are important tools both for calibrating analytical templates for gravitational-wave detection and for exploring the nonlinear dynamics of curved spacetime. However, all previous simulations of binary-black-hole inspiral, merger, and ringdown have been limited by an apparently insurmountable barrier: the merging holes' spins could not exceed 0.93, which is still a long way from the maximum possible value in terms of the physical effects of the spin. In this paper, we surpass this limit for the first time, opening the way to explore numerically the behavior of merging, nearly extremal black holes. Specifically, using an improved initial-data method suitable for binary black holes with nearly extremal spins, we simulate the inspiral (through 12.5 orbits), merger and ringdown of two equal-mass black holes with equal spins of magnitude 0.95 antialigned with the orbital angular momentum.

  4. Effect of squeezing on parameter estimation of gravitational waves emitted by compact binary systems

    E-Print Network [OSTI]

    Ryan Lynch; Salvatore Vitale; Lisa Barsotti; Matthew Evans; Sheila Dwyer

    2014-11-06T23:59:59.000Z

    The LIGO gravitational wave (GW) detectors will begin collecting data in 2015, with Virgo following shortly after. The use of squeezing has been proposed as a way to reduce the quantum noise without increasing the laser power, and has been successfully tested at one of the LIGO sites and at GEO in Germany. When used in Advanced LIGO without a filter cavity, the squeezer improves the performances of detectors above about 100 Hz, at the cost of a higher noise floor in the low frequency regime. Frequency-dependent squeezing, on the other hand, will lower the noise floor throughout the entire band. Squeezing technology will have a twofold impact: it will change the number of expected detections and it will impact the quality of parameter estimation for the detected signals. In this work we consider three different GW detector networks, each utilizing a different type of squeezer, all corresponding to plausible implementations. Using LALInference, a powerful Monte Carlo parameter estimation algorithm, we study how each of these networks estimates the parameters of GW signals emitted by compact binary systems, and compare the results with a baseline advanced LIGO-Virgo network. We find that, even in its simplest implementation, squeezing has a large positive impact: the sky error area of detected signals will shrink by about 30% on average, increasing the chances of finding an electromagnetic counterpart to the GW detection. Similarly, we find that the measurability of tidal deformability parameters for neutron stars in binaries increases by about 30%, which could aid in determining the equation of state of neutron stars. The degradation in the measurement of the chirp mass, as a result of the higher low-frequency noise, is shown to be negligible when compared to systematic errors.

  5. Fast and accurate prediction of numerical relativity waveforms from binary black hole mergers using surrogate models

    E-Print Network [OSTI]

    Jonathan Blackman; Scott E. Field; Chad R. Galley; Bela Szilagyi; Mark A. Scheel; Manuel Tiglio; Daniel A. Hemberger

    2015-02-26T23:59:59.000Z

    Simulating a binary black hole coalescence by solving Einstein's equations is computationally expensive, requiring days to months of supercomputing time. In this paper, we construct an accurate and fast-to-evaluate surrogate model for numerical relativity (NR) waveforms from non-spinning binary black hole coalescences with mass ratios from $1$ to $10$ and durations corresponding to about $15$ orbits before merger. Our surrogate, which is built using reduced order modeling techniques, is distinct from traditional modeling efforts. We find that the full multi-mode surrogate model agrees with waveforms generated by NR to within the numerical error of the NR code. In particular, we show that our modeling strategy produces surrogates which can correctly predict NR waveforms that were {\\em not} used for the surrogate's training. For all practical purposes, then, the surrogate waveform model is equivalent to the high-accuracy, large-scale simulation waveform but can be evaluated in a millisecond to a second depending on the number of output modes and the sampling rate. Our model includes all spherical-harmonic ${}_{-2}Y_{\\ell m}$ waveform modes that can be resolved by the NR code up to $\\ell=8$, including modes that are typically difficult to model with other approaches. We assess the model's uncertainty, which could be useful in parameter estimation studies seeking to incorporate model error. We anticipate NR surrogate models to be useful for rapid NR waveform generation in multiple-query applications like parameter estimation, template bank construction, and testing the fidelity of other waveform models.

  6. Compendium of Experimental Cetane Numbers

    SciTech Connect (OSTI)

    Yanowitz, J.; Ratcliff, M. A.; McCormick, R. L.; Taylor, J. D.; Murphy, M. J.

    2014-08-01T23:59:59.000Z

    This report is an updated version of the 2004 Compendium of Experimental Cetane Number Data and presents a compilation of measured cetane numbers for pure chemical compounds. It includes all available single compound cetane number data found in the scientific literature up until March 2014 as well as a number of unpublished values, most measured over the past decade at the National Renewable Energy Laboratory. This Compendium contains cetane values for 389 pure compounds, including 189 hydrocarbons and 201 oxygenates. More than 250 individual measurements are new to this version of the Compendium. For many compounds, numerous measurements are included, often collected by different researchers using different methods. Cetane number is a relative ranking of a fuel's autoignition characteristics for use in compression ignition engines; it is based on the amount of time between fuel injection and ignition, also known as ignition delay. The cetane number is typically measured either in a single-cylinder engine or a constant volume combustion chamber. Values in the previous Compendium derived from octane numbers have been removed, and replaced with a brief analysis of the correlation between cetane numbers and octane numbers. The discussion on the accuracy and precision of the most commonly used methods for measuring cetane has been expanded and the data has been annotated extensively to provide additional information that will help the reader judge the relative reliability of individual results.

  7. Collective properties of neutron-star X-ray binary populations of galaxies. II. Pre-low-mass X-ray binary properties, formation rates, and constraints

    SciTech Connect (OSTI)

    Bhadkamkar, H. [Astronomy and Astrophysics, Raman Research Institute, Bengaluru 560080 (India); Ghosh, P. [Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Mumbai 400005 (India)

    2014-04-01T23:59:59.000Z

    We continue our exploration of the collective properties of neutron-star X-ray binaries in the stellar fields (i.e., outside globular clusters) of normal galaxies. In Paper I of this series, we considered high-mass X-ray binaries (HMXBs). In this paper (Paper II), we consider low-mass X-ray binaries (LMXBs), whose evolutionary scenario is very different from that of HMXBs. We consider the evolution of primordial binaries up to the stage where the neutron star just formed in the supernova explosion of the primary is in a binary with its low-mass, unevolved companion, and this binary has circularized tidally, producing what we call a pre-low-mass X-ray binary (pre-LMXB). We study the constraints on the formation of such pre-LMXBs in detail (since these are low-probability events), and calculate their collective properties and formation rates. To this end, we first consider the changes in the binary parameters in the various steps involved, viz., the common-envelope phase, the supernova, and the tidal evolution. This naturally leads to a clarification of the constraints. We then describe our calculation of the evolution of the distributions of primordial binary parameters into those of pre-LMXB parameters, following the standard evolutionary scenario for individual binaries. We display the latter as both bivariate and monovariate distributions, discuss their essential properties, and indicate the influences of some essential factors on these. Finally, we calculate the formation rate of these pre-LMXBs. The results of this paper will be used in a subsequent one to compute the expected X-ray luminosity function of LMXBs.

  8. FM stars II: a Fourier view of pulsating binary stars -- determining binary orbital parameters photometrically for highly eccentric cases

    E-Print Network [OSTI]

    Shibahashi, Hiromoto; Murphy, Simon J

    2015-01-01T23:59:59.000Z

    Continuous and precise space-based photometry has made it possible to measure the orbital frequency modulation of pulsating stars in binary systems with extremely high precision over long time spans. Frequency modulation caused by binary orbital motion manifests itself as a multiplet with equal spacing of the orbital frequency in the Fourier transform. The amplitudes and phases of the peaks in these multiplets reflect the orbital properties, hence the orbital parameters can be extracted by analysing such precise photometric data alone. We derive analytically the theoretical relations between the multiplet properties and the orbital parameters, and present a method for determining these parameters, including the eccentricity and the argument of periapsis, from a quintuplet or a higher order multiplet. This is achievable with the photometry alone, without spectroscopic radial velocity measurements. We apply this method to Kepler mission data of KIC8264492, KIC9651065, and KIC10990452, each of which is shown to ...

  9. Number

    Office of Legacy Management (LM)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645 3,625 1,006 492 742EnergyOn AprilA groupTuba City, Arizona, DisposalFourthN V O 1 8 7 +New York, New

  10. Brookhaven National Laboratory Number: Revision

    E-Print Network [OSTI]

    Ohta, Shigemi

    Brookhaven National Laboratory Number: Revision: PS-ESH-0057 01 Effective: Page 1 of 9 06 Chris Weilandics Signature on file Department ES&H Approval printed name Signature Date Lori Stiegler Signature on file #12;Number: PS-ESH-0057 Revision: 01 Effective: 06/08/12 Page 2 of 9 The only official

  11. A new method of determining the inclination angle in interacting binaries

    E-Print Network [OSTI]

    Tariq Shahbaz

    1998-03-25T23:59:59.000Z

    We describe a method of determining the system parameters in non-eclipsing interacting binaries. We find that the extent to which an observer sees the shape of the Roche-lobe of the secondary star governs the amount of distortion of the absorption line profiles. The width and degree of asymmetry of the phase-resolved absorption line profiles show a characteristic shape, which depends primarily on the binary inclination and gravity darkening exponent. We show that, in principle, by obtaining high spectral and time resolution spectra of quiescent cataclysmic variables or low mass X-ray binaries in which the mass-losing star is visible, fitting the shape of absorption line profiles will allow one to determine not only the mass function of the binary, but also the binary inclination and hence the mass of the binary components.

  12. Binary microlensing event OGLE-2009-BLG-020 gives a verifiable mass, distance and orbit predictions

    E-Print Network [OSTI]

    Skowron, J; Gould, A; Dong, Subo; Monard, L A G; Han, C; Nelson, C R; McCormick, J; Moorhouse, D; Thornley, G; Maury, A; Bramich, D M; Greenhill, J; Kozlowski, S; Bond, I; Poleski, R; Wyrzykowski, L; Ulaczyk, K; Kubiak, M; Szymanski, M K; Pietrzynski, G; Soszynski, I; Gaudi, B S; Yee, J C; Hung, L -W; Pogge, R W; DePoy, D L; Lee, C -U; Park, B -G; Allen, W; Mallia, F; Drummond, J; Bolt, G; Allan, A; Browne, P; Clay, N; Dominik, M; Fraser, S; Horne, K; Kains, N; Mottram, C; Snodgrass, C; Steele, I; Street, R A; Tsapras, Y; Abe, F; Bennett, D P; Botzler, C S; Douchin, D; Freeman, M; Fukui, A; Furusawa, K; Hayashi, F; Hearnshaw, J B; Hosaka, S; Itow, Y; Kamiya, K; Kilmartin, P M; Korpela, A; Lin, W; Ling, C H; Makita, S; Masuda, K; Matsubara, Y; Muraki, Y; Nagayama, T; Miyake, N; Nishimoto, K; Ohnishi, K; Perrott, Y C; Rattenbury, N; Saito, To; Skuljan, L; Sullivan, D J; Sumi, T; Suzuki, D; Sweatman, W L; Tristram, P J; Wada, K; Yock, P C M; Beaulieu, J -P; Fouque, P; Albrow, M D; Batista, V; Brillant, S; Caldwell, J A R; Cassan, A; Cole, A; Cook, K H; Coutures, Ch; Dieters, S; Prester, D Dominis; Donatowicz, J; Kane, S R; Kubas, D; Marquette, J -B; Martin, R; Menzies, J; Sahu, K C; Wambsganss, J; Williams, A; Zub, M

    2011-01-01T23:59:59.000Z

    We present the first example of binary microlensing for which the parameter measurements can be verified (or contradicted) by future Doppler observations. This test is made possible by a confluence of two relatively unusual circumstances. First, the binary lens is bright enough (I=15.6) to permit Doppler measurements. Second, we measure not only the usual 7 binary-lens parameters, but also the 'microlens parallax' (which yields the binary mass) and two components of the instantaneous orbital velocity. Thus we measure, effectively, 6 'Kepler+1' parameters (two instantaneous positions, two instantaneous velocities, the binary total mass, and the mass ratio). Since Doppler observations of the brighter binary component determine 5 Kepler parameters (period, velocity amplitude, eccentricity, phase, and position of periapsis), while the same spectroscopy yields the mass of the primary, the combined Doppler + microlensing observations would be overconstrained by 6 + (5 + 1) - (7 + 1) = 4 degrees of freedom. This mak...

  13. The Equations of Motion of Compact Binaries in the Neighborhood of Supermassive Black Hole

    SciTech Connect (OSTI)

    Gorbatsievich, Alexander; Bobrik, Alexey [Belarusian state university, Nezavisimosti Av., 4, 220030 Minsk (Belarus)

    2010-03-24T23:59:59.000Z

    By the use of Einstein-Infeld-Hoffmann method, the equations of motion of a binary star system in the field of a supermassive black hole are derived. In spite of the fact that the motion of a binary system as a whole can be relativistic or even ultra-relativistic with respect to the supermassive black hole, it is shown, that under the assumption of non-relativistic relative motion of the stars in binary system, the motion of the binary system as a whole satisfies the Mathisson-Papapetrou equations with additional terms depending on quadrupole moments. Exemplary case of ultrarelativistic motion of a binary neutron star in the vicinity of non-rotating black hole is considered. It it shown that the motion of binary's center of mass may considerably differ from geodesic motion.

  14. Automated eclipsing binary detection: applying the Gaia CU7 pipeline to Hipparcos

    E-Print Network [OSTI]

    Holl, Berry; Lecoeur-Taïbi, Isabelle; Barblan, Fabio; Rimoldini, Lorenzo; Eyer, Laurent; Süveges, Maria; Guy, Leanne; Ordoñez-Blanco, Diego; Ruiz, Idoia; Nienartowicz, Krzysztof

    2015-01-01T23:59:59.000Z

    We demonstrate the eclipsing binary detection performance of the Gaia variability analysis and processing pipeline using Hipparcos data. The automated pipeline classifies 1,067 (0.9%) of the 118,204 Hipparcos sources as eclipsing binary candidates. The detection rate amounts to 89% (732 sources) in a subset of 819 visually confirmed eclipsing binaries, with the period correctly identified for 80% of them, and double or half periods obtained in 6% of the cases.

  15. Isobaric vapor-liquid equilibria for methanol + ethanol + water and the three constituent binary systems

    SciTech Connect (OSTI)

    Kurihara, Kiyofumi; Nakamichi, Mikiyoshi; Kojima, Kazuo (Nihon Univ., Tokyo (Japan). Dept. of Industrial Chemistry)

    1993-07-01T23:59:59.000Z

    Vapor-liquid equilibrium data for methanol + ethanol + water and its three constituent binary systems methanol + ethanol, ethanol + water, and methanol + water were measured at 101.3 kPa using a liquid-vapor ebullition-type equilibrium still. The experimental binary data were correlated by the NRTL equation. The ternary system methanol + ethanol + water was predicted by means of the binary NRTL parameters with good accuracy.

  16. Weight Distribution of a Class of Binary Linear Block Codes Formed from RCPC Codes

    E-Print Network [OSTI]

    Shen, Yushi Dr.; Cosman, Pamela C; Milstein, Laurence B

    2006-01-01T23:59:59.000Z

    On the weight distribution of terminated convolutionalViterbi, “On the weight distribution of linear block codes9, SEPTEMBER 2005 Weight Distribution of a Class of Binary

  17. A Type System for Certified Binaries Zhong Shao Bratin Saha Valery Trifonov Nikolaos Papaspyr*

    E-Print Network [OSTI]

    for Certified Binaries Zhong Shao Bratin Saha Valery Trifonov Nikolaos Papaspyr* *ou.S.A. {shao, saha, trifonov, nickie}@cs.yale.edu Abstract ever, none

  18. Migration of massive black hole binaries in self--gravitating accretion discs: Retrograde versus prograde

    E-Print Network [OSTI]

    Constanze Roedig; Alberto Sesana

    2013-07-24T23:59:59.000Z

    We study the interplay between mass transfer, accretion and gravitational torques onto a black hole binary migrating in a self-gravitating, retrograde circumbinary disc. A direct comparison with an identical prograde disc shows that: (i) because of the absence of resonances, the cavity size is a factor a(1+e) smaller for retrograde discs; (ii) nonetheless the shrinkage of a circular binary semi--major axis, a, is identical in both cases; (iii) a circular binary in a retrograde disc remains circular while eccentric binaries grow more eccentric. For non-circular binaries, we measure the orbital decay rates and the eccentricity growth rates to be exponential as long as the binary orbits in the plane of its disc. Additionally, for these co-planar systems, we find that interaction (~ non--zero torque) stems only from the cavity edge plus a(1+e) in the disc, i.e. for dynamical purposes, the disc can be treated as a annulus of small radial extent. We find that simple 'dust' models in which the binary- disc interaction is purely gravitational can account for all main numerical results, both for prograde and retrograde discs. Furthermore, we discuss the possibility of an instability occurring for highly eccentric binaries causing it to leave the disc plane, secularly tilt and converge to a prograde system. Our results suggest that there are two stable configurations for binaries in self-gravitating discs: the special circular retrograde case and an eccentric (e~ 0.6) prograde configuration as a stable attractor.

  19. Departmental Business Instrument Numbering System

    Broader source: Directives, Delegations, and Requirements [Office of Management (MA)]

    2000-12-05T23:59:59.000Z

    To prescribe procedures for assigning identifying numbers to all Department of Energy (DOE), including the National Nuclear Security Administration, business instruments. Cancels DOE 1331.2B. Canceled by DOE O 540.1A.

  20. Departmental Business Instrument Numbering System

    Broader source: Directives, Delegations, and Requirements [Office of Management (MA)]

    2005-01-27T23:59:59.000Z

    The Order prescribes the procedures for assigning identifying numbers to all Department of Energy (DOE) and National Nuclear Security Administration (NNSA) business instruments. Cancels DOE O 540.1. Canceled by DOE O 540.1B.

  1. The Jacobi-Stirling Numbers

    E-Print Network [OSTI]

    Andrews, George E; Gawronski, Wolfgang; Littlejohn, Lance L

    2011-01-01T23:59:59.000Z

    The Jacobi-Stirling numbers were discovered as a result of a problem involving the spectral theory of powers of the classical second-order Jacobi differential expression. Specifically, these numbers are the coefficients of integral composite powers of the Jacobi expression in Lagrangian symmetric form. Quite remarkably, they share many properties with the classical Stirling numbers of the second kind which, as shown in LW, are the coefficients of integral powers of the Laguerre differential expression. In this paper, we establish several properties of the Jacobi-Stirling numbers and its companions including combinatorial interpretations thereby extending and supplementing known contributions to the literature of Andrews-Littlejohn, Andrews-Gawronski-Littlejohn, Egge, Gelineau-Zeng, and Mongelli.

  2. SELF-REGULATED SHOCKS IN MASSIVE STAR BINARY SYSTEMS

    SciTech Connect (OSTI)

    Parkin, E. R.; Sim, S. A., E-mail: parkin@mso.anu.edu.au, E-mail: s.sim@qub.ac.uk [Research School of Astronomy and Astrophysics, Australian National University, ACT 2611 (Australia)

    2013-04-20T23:59:59.000Z

    In an early-type, massive star binary system, X-ray bright shocks result from the powerful collision of stellar winds driven by radiation pressure on spectral line transitions. We examine the influence of the X-rays from the wind-wind collision shocks on the radiative driving of the stellar winds using steady-state models that include a parameterized line force with X-ray ionization dependence. Our primary result is that X-ray radiation from the shocks inhibits wind acceleration and can lead to a lower pre-shock velocity, and a correspondingly lower shocked plasma temperature, yet the intrinsic X-ray luminosity of the shocks, L{sub X}, remains largely unaltered, with the exception of a modest increase at small binary separations. Due to the feedback loop between the ionizing X-rays from the shocks and the wind driving, we term this scenario as self-regulated shocks. This effect is found to greatly increase the range of binary separations at which a wind-photosphere collision is likely to occur in systems where the momenta of the two winds are significantly different. Furthermore, the excessive levels of X-ray ionization close to the shocks completely suppress the line force, and we suggest that this may render radiative braking less effective. Comparisons of model results against observations reveal reasonable agreement in terms of log (L{sub X}/L{sub bol}). The inclusion of self-regulated shocks improves the match for kT values in roughly equal wind momenta systems, but there is a systematic offset for systems with unequal wind momenta (if considered to be a wind-photosphere collision).

  3. A Search for Eclipsing Binaries in Galactic Globular Clusters

    E-Print Network [OSTI]

    Kaspar von Braun

    2003-01-22T23:59:59.000Z

    We report on the discovery and analysis of short-period (0.1 days $< P <$ 5 days), photometrically varying binary stars around and below the main-sequence turnoff of the globular clusters (GCs) NGC 3201, M10, & M12. These eclipsing binaries (EBs) may be used to determine directly the distances to GCs and constrain the Population II stellar main-sequence masses. During our search for binaries, we discovered the signature of differential reddening across the cluster fields which was especially strong for NGC 3201 and M10. We correct for this differential reddening by calculating average $E_{V-I}$ values for stars in small subregions of the field with respect to a fiducial region, which significantly improves the appearance of the GC color-magnitude diagrams (CMDs). The reddening zero point to be added to the differential value is determined by isochrone fitting. The results of our differential dereddening are presented in the form of high-resolution extinction maps. Our search for EBs returned 14 variable stars (11 EBs) in the field of NGC 3201, 3 variables (1 EB) in M10, and 2 EBs in M12. Of these variables, only one EB in NGC 3201 (a blue straggler W Ursa Majoris contact system) is a definite GC-member, based on spectroscopic observations. Another W UMa contact EB in M12 is most likely a member of M12, based on its location in the color-magnitude diagram (CMD) and its empirically calculated absolute magnitude. We present the phased lightcurves for all variables, estimate their distances and GC membership, and show their locations in the GC fields and CMDs, as well as the spectra of the NGC 3201 EBs. Finally, we discuss the implications of our results and outline future work.

  4. Wind accretion in binary stars II. Accretion rates

    E-Print Network [OSTI]

    Tom Theuns; Henri Boffin; Alain Jorissen

    1996-02-18T23:59:59.000Z

    Smoothed particle hydrodynamics (SPH) is used to estimate accretion rates of mass, linear and angular momentum in a binary system where one component undergoes mass loss through a wind. Physical parameters are chosen such as to model the alleged binary precursors of barium stars, whose chemical peculiarities are believed to result from the accretion of the wind from a companion formerly on the asymptotic giant branch (AGB). The binary system modelled consists of a 3 solar masses AGB star on the main sequence, in a 3AU circular orbit. Three-dimensional simulations are performed for gases with polytropic indices gamma=1, 1.1 and 1.5, to bracket more realistic situations that would include radiative cooling. Mass accretion rates are found to depend on resolution and we estimate typical values of 1-2% for the gamma=1.5 case and 8% for the other models. The highest resolution obtained (with 400k particles) corresponds to an accretor of linear size 16 solar radii. Despite being (in the gamma = 1.5 case) about ten times smaller than theoretical estimates based on the Bondi-Hoyle prescription, the SPH accretion rates remain large enough to explain the pollution of barium stars. Uncertainties in the current SPH rates remain however, due to the simplified treatment of the wind acceleration mechanism, as well as to the absence of any cooling prescription and to the limited numerical resolution. Angular momentum transfer leads to significant spin up of the accretor and can account for the rapid rotation of HD165141, a barium star with a young white dwarf companion and a rotation rate unusually large among K giants.

  5. Revisit on ''Ruling out chaos in compact binary systems''

    SciTech Connect (OSTI)

    Wu Xin [Department of Physics, Nanchang University, Nanchang 330031 (China); Xie Yi [Department of Astronomy, Nanjing University, Nanjing 210093 (China)

    2007-12-15T23:59:59.000Z

    Full general relativity requires that chaos indicators should be invariant in various spacetime coordinate systems for a given relativistic dynamical problem. On the basis of this point, we calculate the invariant Lyapunov exponents (LEs) for one of the spinning compact binaries in the conservative second post-Newtonian (2PN) Lagrangian formulation without the dissipative effects of gravitational radiation, using the two-nearby-orbits method with projection operations and with coordinate time as an independent variable. It is found that the actual source leading to zero LEs in one paper [J. D. Schnittman and F. A. Rasio, Phys. Rev. Lett. 87, 121101 (2001)] but to positive LEs in the other [N. J. Cornish and J. Levin, Phys. Rev. Lett. 89, 179001 (2002)] does not mainly depend on rescaling, but is due to two slightly different treatments of the LEs. It takes much more CPU time to obtain the stabilizing limit values as reliable values of LEs for the former than to get the slopes (equal to LEs) of the fit lines for the latter. Due to coalescence of some of the black holes, the LEs from the former are not an adaptive indicator of chaos for comparable mass compact binaries. In this case, the invariant fast Lyapunov indicator (FLI) of two-nearby orbits, as a very sensitive tool to distinguish chaos from order, is worth recommending. As a result, we do again find chaos in the 2PN approximation through different ratios of FLIs varying with time. Chaos cannot indeed be ruled out in real binaries.

  6. Period Change of Eclipsing Binaries from the ASAS Catalog

    E-Print Network [OSTI]

    Radoslaw Poleski; Bogumil Pilecki

    2006-07-10T23:59:59.000Z

    We present a preliminary statistical analysis of a period change of eclipsing binaries from the ASAS Catalog of Variable Stars. For each contact and semidetached system brighter than 13.3$mag$ (in V) with a period shorter than 0.4 days and at least 300 observation points we have found an angular velocity $\\omega$ and its time derivative $\\frac{d\\omega}{dt}$. According to our accuracy there is no evidence that average $\\frac{d\\omega}{dt}$ differs from 0. Light curves for selected stars are presented.

  7. Plastic flow in polycrystal states in a binary mixture

    E-Print Network [OSTI]

    Toshiyuki Hamanaka; Akira Onuki

    2007-09-05T23:59:59.000Z

    Using molecular dynamics simulation we examine dynamics in sheared polycrystal states in a binary mixture containing 10% larger particles in two dimensions. We find large stress fluctuations arising from sliding motions of the particles at the grain boundaries, which occur cooperatively to release the elastic energy stored. These dynamic processes are visualized with the aid of a sixfold angle $\\alpha_j(t)$ representing the local crystal orientation and a disorder variable $D_j(t)$ representing a deviation from the hexagonal order for particle $j$.

  8. Binary vapor-liquid equilibrium data without measurement of composition

    E-Print Network [OSTI]

    Nehzat, Mohammad Sadegh

    1975-01-01T23:59:59.000Z

    . Blak- ley for their assistance in serving as committee members and for their constructive criticisms of this thesis. The help rendered by Mr. B. Bala)i Singh in typing this thesis is appreciated. vii TABLE OF CONTENTS ABSTRACT. ACKNOWLZDGEMENTS...NUZ DO 300 J=1, NT NPV=NP(J, N) READ(MR, 100) (V(I)=1&NPV) FORMAT(5F10 ~ 5) NPP=NP(J, N) DO 301 I=1, NPP RHO(I, J, N)=1. 00/V(I) GONTINUZ THIS PART READS DATA FOR SATURATION ENVELOPES OF EACH BINARY MIXTURE READ& KMINS(N) & KMAXS(N) KMINT...

  9. A Flashing Binary Combined Cycle For Geothermal Power Generation | Open

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page onYou are now leaving Energy.gov You are now leaving Energy.gov You are beingZealand Jump to:Ezfeedflag JumpID-fTriWildcat 1 WindtheEnergy Information Flashing Binary Combined Cycle

  10. Mahanagdong B-Binary GEPP | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page onYou are now leaving Energy.gov You are now leaving Energy.gov YouKizildere I Geothermal Pwer Plant Jump to:LandownersLuther,Jemez Pueblo Area (DOE GTP)Texas: EnergyMahanagdong AB-Binary

  11. Mak-Ban Binary 2 GEPP | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page onYou are now leaving Energy.gov You are now leaving Energy.gov YouKizildere I Geothermal Pwer Plant Jump to:LandownersLuther,Jemez Pueblo Area (DOEMak-Ban / Laguna Geothermal AreaBinary

  12. Statistics & Gene Expression Data Analysis Note 8: Binary Regression Outcomes and classification probabilities

    E-Print Network [OSTI]

    West, Mike

    classification, validation, prognosis Binary regression models · Linear regression model based on regression ­ Standard statistical models transform from real-value to (0, 1) using a specified non-linear functionStatistics & Gene Expression Data Analysis Note 8: Binary Regression Outcomes and classification

  13. WIND TOMOGRAPHY IN BINARY SYSTEMS O.Knill, R.Dgani and M.Vogel

    E-Print Network [OSTI]

    Knill, Oliver

    WIND TOMOGRAPHY IN BINARY SYSTEMS O.Knill, R.Dgani and M.Vogel ETH-Zurich, CH-8092, Switzerland method is particularly suitable for determining the velocity laws of stellar winds. 1. WIND TOMOGRAPHY AND ABEL'S INTEGRAL Binary systems in which a compact, point-like radiation source shines through the wind

  14. SIMULATION OF STRESSES DURING CASTING OF BINARY MAGNESIUM-ALUMINUM ALLOYS M.G. Pokorny1

    E-Print Network [OSTI]

    Beckermann, Christoph

    SIMULATION OF STRESSES DURING CASTING OF BINARY MAGNESIUM-ALUMINUM ALLOYS M.G. Pokorny1 , C, Geesthacht, Germany Keywords: Magnesium Alloys, Casting, Stress Simulation Abstract A visco-plastic deformation model is used to predict thermal stresses during casting of binary Mg-Al alloys. The predictions

  15. The Binary Energy Harvesting Channel with a Unit-Sized Battery

    E-Print Network [OSTI]

    Ulukus, Sennur

    by the exogenous energy harvesting process, energy storage capacity of the battery, and the past channel inputs1 The Binary Energy Harvesting Channel with a Unit-Sized Battery Kaya Tutuncuoglu1 , Omur Ozel2 a binary energy harvesting communication channel with a finite-sized battery at the transmitter

  16. K-means Hashing: an Affinity-Preserving Quantization Method for Learning Binary Compact Codes

    E-Print Network [OSTI]

    Bernstein, Phil

    K-means Hashing: an Affinity-Preserving Quantization Method for Learning Binary Compact Codes. In this paper, we present a hashing method adopting the k-means quantization. We propose a novel Affinity-Preserving K-means algorithm which simultane- ously performs k-means clustering and learns the binary indices

  17. CRYSTALLINE SILICATE EMISSION IN THE PROTOSTELLAR BINARY SERPENS SVS 20 David R. Ciardi

    E-Print Network [OSTI]

    De Buizer, James Michael

    CRYSTALLINE SILICATE EMISSION IN THE PROTOSTELLAR BINARY SERPENS SVS 20 David R. Ciardi Michelson near 11.3 m, while SVS 20-North exhibits a shallow amorphous silicate absorption spectrum with a peak 20-S and SVS 20-N. The presence of crystalline silicate in such a young binary system indicates

  18. CRYSTALLINE SILICATE EMISSION IN THE PROTOSTELLAR BINARY SERPENS SVS 20 David R. Ciardi

    E-Print Network [OSTI]

    De Buizer, James Michael

    CRYSTALLINE SILICATE EMISSION IN THE PROTOSTELLAR BINARY SERPENS SVS 20 David R. Ciardi Michelson near 11.3 #m, while SVS 20­North exhibits a shallow amorphous silicate absorption spectrum with a peak 20­S and SVS 20­N. The presence of crystalline silicate in such a young binary system indicates

  19. Testing Closed-Source Binary Device Drivers with DDT Volodymyr Kuznetsov, Vitaly Chipounov, and George Candea

    E-Print Network [OSTI]

    Candea, George

    Testing Closed-Source Binary Device Drivers with DDT Volodymyr Kuznetsov, Vitaly Chipounov (EPFL), Switzerland Abstract DDT is a system for testing closed-source binary de- vice drivers against think of it as a pesticide against device driver bugs. DDT combines virtualization with a spe- cialized

  20. VAPOR + LIQUID EQUILIBRIUM OF WATER, CARBON DIOXIDE, AND THE BINARY SYSTEM WATER + CARBON DIOXIDE FROM

    E-Print Network [OSTI]

    ) and their binary mixtures (between 348 and 393 K). The properties of supercritical carbon dioxide were determinedVAPOR + LIQUID EQUILIBRIUM OF WATER, CARBON DIOXIDE, AND THE BINARY SYSTEM WATER + CARBON DIOXIDE the vapor-liquid equilibrium of water (between 323 and 573 K), carbon dioxide (between 230 and 290 K

  1. Turbo Codes for Binary Markov Sources 1 Guang-Chong Zhu and Fady Alajaji

    E-Print Network [OSTI]

    Linder, Tamás

    Turbo Codes for Binary Markov Sources 1 Guang-Chong Zhu and Fady Alajaji Dept. of Mathematics@mast.queensu.ca Abstract | The reliable transmission via Turbo codes of binary stationary ergodic Markov sources over noisy channels is investigated. The #12;rst con- stituent Turbo decoder is designed to exploit the source

  2. DIVISION S-2-SOIL CHEMISTRY Acetonitrile and Acrylonitrile Sorption on Montmorillonite from Binary

    E-Print Network [OSTI]

    Sparks, Donald L.

    DIVISION S-2-SOIL CHEMISTRY Acetonitrile and Acrylonitrile Sorption on Montmorillonite from Binary of acetonitrile and acrylonitrile on K, Na, Ca, and Mg montmorillonite from binary and ternary aqueous solutions that the sorption of acetonitrile and acrylonitrile from ternary solutions on K montmorillonite was competitive

  3. Planetary Nebulae Principles & Paradigms: Binaries, Accretion, Magnetic Fields

    E-Print Network [OSTI]

    Eric G. Blackman; Jason T. Nordhaus

    2007-10-01T23:59:59.000Z

    Observations suggest that many, if not all, post AGB systems evolve through an aspherical outflow phase. Such outflows require a sufficient engine rotational energy which binaries can provide. Via common envelope evolution, binaries can directly eject equatorial outflows or produce poloidal outflows from magnetized accretion disks around the primary or secondary. We discuss how accretion driven magnetohydrodynamic outflow models all make similar predictions for the outflow power and speed and we distinguish between the launch vs. propagation regimes of such outflows. We suggest that the high velocity bipolar outflows observed in planetary nebulae (PNe) and the lower velocity but higher power bipolar outflows observed in pre-PNe (pPNe) are kinematically consistent with time dependent accretion onto a white dwarf (WD) within a depleting envelope. Since the WD primary core is always present in all post-AGB systems, accretion onto this core is potentially common. Previous work has focused on core accretion from sub-stellar companions, but low mass stellar companions may be more important, and further work is needed.

  4. FORMATION OF STABLE MAGNETARS FROM BINARY NEUTRON STAR MERGERS

    SciTech Connect (OSTI)

    Giacomazzo, Bruno [JILA, University of Colorado and National Institute of Standards and Technology, Boulder, CO 80309 (United States); Perna, Rosalba [JILA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309 (United States)

    2013-07-10T23:59:59.000Z

    By performing fully general relativistic magnetohydrodynamic simulations of binary neutron star mergers, we investigate the possibility that the end result of the merger is a stable magnetar. In particular, we show that, for a binary composed of two equal-mass neutron stars (NSs) of gravitational mass M {approx} 1.2 M{sub Sun} and equation of state similar to Shen et al. at high densities, the merger product is a stable NS. Such NS is found to be differentially rotating and ultraspinning with spin parameter J/M{sup 2} {approx} 0.86, where J is its total angular momentum, and it is surrounded by a disk of Almost-Equal-To 0.1 M{sub Sun }. While in our global simulations the magnetic field is amplified by about two orders of magnitude, local simulations have shown that hydrodynamic instabilities and the onset of the magnetorotational instability could further increase the magnetic field strength up to magnetar levels. This leads to the interesting possibility that, for some NS mergers, a stable and magnetized NS surrounded by an accretion disk could be formed. We discuss the impact of these new results for the emission of electromagnetic counterparts of gravitational wave signals and for the central engine of short gamma-ray bursts.

  5. Theoretical X-ray Line Profiles from Colliding Wind Binaries

    E-Print Network [OSTI]

    D. B. Henley; I. R. Stevens; J. M. Pittard

    2003-06-23T23:59:59.000Z

    We present theoretical X-ray line profiles from a range of model colliding wind systems. In particular, we investigate the effects of varying the stellar mass-loss rates, the wind speeds, and the viewing orientation. We find that a wide range of theoretical line profile shapes is possible, varying with orbital inclination and phase. At or near conjunction, the lines have approximately Gaussian profiles, with small widths (HWHM ~ 0.1 v_\\infty) and definite blue- or redshifts (depending on whether the star with the weaker wind is in front or behind). When the system is viewed at quadrature, the lines are generally much broader (HWHM ~ v_\\infty), flat-topped and unshifted. Local absorption can have a major effect on the observed profiles - in systems with mass-loss rates of a few times 10^{-6} Msol/yr the lower energy lines (E wind of the primary. The orbital variation of the line widths and shifts is reduced in a low inclination binary. The extreme case is a binary with i = 0 degrees, for which we would expect no line profile variation.

  6. TeV neutrinos from microquasars in compact massive binaries

    E-Print Network [OSTI]

    W. Bednarek

    2005-05-27T23:59:59.000Z

    We consider a compact binary system in which a Wolf-Rayet star supplies matter onto a stellar mass black hole or a neutron star. This matter forms an accretion disk which ejects a jet as observed in Galactic microquasars. A part of the jet kinetic energy, typically 10%, can be transfered to relativistic nuclei. These nuclei lose nucleons as a result of photo-disintegration process in collisions with thermal photons from the accretion disk and the massive star. Due to the head on photon-nucleus collisions most of neutrons released from nuclei move towards the surface of the accretion disk and/or the massive star producing neutrinos in collisions with the matter. We calculate the spectra of muon neutrinos and expected neutrino event rates in a 1 km^2 neutrino detector of the IceCube type from a microquasar inside our Galaxy applying, as an example, the parameters of the Cyg X-3 binary system, provided that nuclei are accelerated to the Lorentz factors above 10^6 with the power law spectrum with an index close to 2.

  7. Simulations of black hole-neutron star binary coalescence

    E-Print Network [OSTI]

    William H. Lee

    2001-01-09T23:59:59.000Z

    We show the results of dynamical simulations of the coalescence of black hole-neutron star binaries. We use a Newtonian Smooth Particle Hydrodynamics code, and include the effects of gravitational radiation back reaction with the quadrupole approximation for point masses, and compute the gravitational radiation waveforms. We assume a polytropic equation of state determines the structure of the neutron star in equilibrium, and use an ideal gas law to follow the dynamical evolution. Three main parameters are explored: (i) The distribution of angular momentum in the system in the initial configuration, namely tidally locked systems vs. irrotational binaries; (ii) The stiffness of the equation of state through the value of the adiabatic index Gamma (ranging from Gamma=5/3 to Gamma=3); (iii) The initial mass ratio q=M(NS)/M(BH). We find that it is the value of Gamma that determines how the coalescence takes place, with immediate and complete tidal disruption for Gamma less than 2, while the core of the neutron star survives and stays in orbit around the black hole for Gamma=3. This result is largely independent of the initial mass ratio and spin configuration, and is reflected directly in the gravitational radiation signal. For a wide range of mass ratios, massive accretion disks are formed (M(disk)~0.2 solar masses), with baryon-free regions that could possibly give rise to gamma ray bursts.

  8. Photometric analysis of the overcontact binary CW Cas

    SciTech Connect (OSTI)

    Wang, J. J.; Qian, S. B.; He, J. J.; Li, L. J.; Zhao, E. G., E-mail: wjjbxw@ynao.ac.cn [National Astronomical Observatories/Yunnan Observatories, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming (China)

    2014-11-01T23:59:59.000Z

    New CCD photometric observations of overcontact binary CW Cas were carried out in 2004 and 2011. In particular, the light curve obtained in 2004 shows a remarkable O'Connell effect. Compared with light curves in different observing seasons, variations were found. These variations can be explained by dark spot activities on the surface of at least one component. Using the Wilson-Devinney code with a spot model, we find that the photometric solutions confirm CW Cas is a shallow W-subtype overcontact binary with a spotted massive component. Our new determined times of minimum light together with the others published in the literature were analyzed to find a change of orbital period. From the O – C curves, the period of the system shows a cyclic period change (P {sub 3} = 69.9 yr, A {sub 3} = 0.03196 days) superposed on the linear increase. The cyclic variation, if explained as the light-travel time effect, reveals the presence of a tertiary companion.

  9. Postirradiation deformation of ferritic Fe-Cr binary alloys

    SciTech Connect (OSTI)

    Hamilton, M.L.; Gelles, D.S.

    1991-06-01T23:59:59.000Z

    Six binary Fe-Cr alloys ranging from 3 to 18% chromium were irradiated in the form of miniature tensile specimens in the Fast Flux Test Facility and tested at room temperature. The irradiation conditions produced 7 to 30 dpa at 365 to 574{degrees}C. The major purpose of the experiment was to compare the behavior of these simple alloys with that of more complex commercial alloys, The tensile data obtained on these specimens at room temperature are discussed with appropriate fractographic and microstructural support. Previous studies on similar materials had revealed the presence of a feature typically exhibited in channel fractures: elongated voids were evident in shear bands of an irradiated and deformed TEM disk of a binary Fe-6Cr alloy. An additional purpose of the experiment was therefore to provide a better understanding of the potential contribution of channel fracture to deformation in ferritic alloys. No evidence for channel fracture was found, however. 14 refs., 6 figs., 2 tabs.

  10. PPl 15 The First Brown Dwarf Spectroscopic Binary

    E-Print Network [OSTI]

    Basri, G S; Basri, Gibor; Martin, Eduardo

    1999-01-01T23:59:59.000Z

    PPl 15 is the first object to have been confirmed as a brown dwarf by the lithium test (in 1995), though its inferred mass was very close to the substellar limit. It is a member of the Pleiades open cluster. Its position in a cluster color-magnitude diagram suggested that it might be binary, and preliminary indications that it is a double-lined spectroscopic binary were reported by us in 1997. Here we report on the results of a consecutive week of Keck HIRES observations of this system, which yield its orbit. It has a period of about 5.8 days, and an eccentricity of 0.4+/-0.05. The rotation of the stars is slow for this class of objects. Because the system luminosity is divided between 2 objects with a mass ratio of 0.85, this renders each of them an incontrovertible brown dwarf, with masses between 60-70 jupiters. We show that component B is a little redder than A by studying their wavelength-dependent line ratios, and that this variation is compatible with the mass ratio. We confirm that the system has lith...

  11. CV evolution: AM Her binaries and the period gap

    E-Print Network [OSTI]

    R. F. Webbink; D. T. Wickramasinghe

    2002-04-19T23:59:59.000Z

    AM Her variables -- synchronised magnetic cataclysmic variables (CVs) -- exhibit a different period distribution from other CVs across the period gap. We show that non-AM Her systems may infiltrate the longer-period end of the period gap if they are metal-deficient, but that the position and width of the gap in orbital period is otherwise insensitive to other binary parameters (excepting the normalisation of the braking rate). In AM Her binaries, magnetic braking is reduced as the wind from the secondary star may be trapped within the magnetosphere of the white dwarf primary. This reduced braking fills the period gap from its short-period end as the dipole magnetic moment of the white dwarf increases. The consistency of these models with the observed distribution of CVs, both AM Her and non-AM Her type, provides compelling evidence supporting magnetic braking as the agent of angular momentum loss among long-period CVs, and its disruption as the explanation of the 2 - 3 hour period gap among nonmagnetic CVs.

  12. Report/Product Number(s) DOE/ER/64701 DOE Award/Contract Number(s)

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645 3,625 1,006 492 742EnergyOnItem Not Found Item Not Foundenhancer activity than FINAL Report/Product Number(s)

  13. Short Gamma Ray Bursts as possible electromagnetic counterpart of coalescing binary systems

    E-Print Network [OSTI]

    S. Capozziello; M. De Laurentis; I. De Martino; M. Formisano

    2010-04-27T23:59:59.000Z

    Coalescing binary systems, consisting of two collapsed objects, are among the most promising sources of high frequency gravitational waves signals detectable, in principle, by ground-based interferometers. Binary systems of Neutron Star or Black Hole/Neutron Star mergers should also give rise to short Gamma Ray Bursts, a subclass of Gamma Ray Bursts. Short-hard-Gamma Ray Bursts might thus provide a powerful way to infer the merger rate of two-collapsed object binaries. Under the hypothesis that most short Gamma Ray Bursts originate from binaries of Neutron Star or Black Hole/Neutron Star mergers, we outline here the possibility to associate short Gamma Ray Bursts as electromagnetic counterpart of coalescing binary systems.

  14. Variation of dispersion measure: evidence of geodetic precession of binary pulsars

    E-Print Network [OSTI]

    B. P. Gong

    2003-06-04T23:59:59.000Z

    Variations of dispersion measure (DM) have been observed in some binary pulsars, which can not be well explained by the propagation effects, such as turbulence of the interstellar media (ISM) between the Earth and the pulsar. This paper provides an alternative interpretation of the phenomena, the geodetic precession of the orbit plane of a binary pulsar system. The dynamic model can naturally avoid the difficulties of propagation explanations. Moreover the additional time delay represented by the DM variation of two binary pulsars can be fitted numerically, through which some interesting parameters of the binary pulsar system, i.e., the moment of inertia of pulsars can be obtained, $I_1=(2.0\\pm0.6)\\times 10^{45}$g cm$^{2}$. The elimination of the additional time delay by the dynamic effect means that ISM between the these pulsars and the Earth might also be stable, like some other binary pulsars.

  15. Isothermal vapor-liquid equilibria for water + 2-aminoethanol + dimethyl sulfoxide and its constituent three binary systems

    SciTech Connect (OSTI)

    Tochigi, Katsumi; Akimoto, Kentarou; Ochi, Kenji [Nihon Univ., Tokyo (Japan). Dept. of Industrial Chemistry] [Nihon Univ., Tokyo (Japan). Dept. of Industrial Chemistry; Liu, Fangyhi; Kawase, Yasuhito [Nippon Refine Co., Ltd., Tokyo (Japan)] [Nippon Refine Co., Ltd., Tokyo (Japan)

    1999-05-01T23:59:59.000Z

    Isothermal vapor-liquid equilibria were measured for the ternary system water + 2-aminoethanol + dimethyl sulfoxide and its three constituent binary mixtures at 363.15 K. The apparatus used was a modified Rogalski-Malanoski equilibrium still. The experimental binary data were correlated by the NRTL equation. The ternary system was predicted using the binary NRTL parameters with good accuracy.

  16. Delayed outflows from black hole accretion tori following neutron star binary coalescence

    E-Print Network [OSTI]

    Rodrigo Fernández; Brian D. Metzger

    2013-07-16T23:59:59.000Z

    Expulsion of neutron-rich matter following the merger of neutron star (NS) binaries is crucial to the radioactively-powered electromagnetic counterparts of these events and to their relevance as sources of r-process nucleosynthesis. Here we explore the long-term (viscous) evolution of remnant black hole accretion disks formed in such mergers by means of two-dimensional, time-dependent hydrodynamical simulations. The evolution of the electron fraction due to charged-current weak interactions is included, and neutrino self-irradiation is modeled as a lightbulb that accounts for the disk geometry and moderate optical depth effects. Over several viscous times (~1s), a fraction ~10% of the initial disk mass is ejected as a moderately neutron-rich wind (Y_e ~ 0.2) powered by viscous heating and nuclear recombination, with neutrino self-irradiation playing a sub-dominant role. Although the properties of the outflow vary in time and direction, their mean values in the heavy-element production region are relatively robust to variations in the initial conditions of the disk and the magnitude of its viscosity. The outflow is sufficiently neutron-rich that most of the ejecta forms heavy r-process elements with mass number A >130, thus representing a new astrophysical source of r-process nucleosynthesis, distinct from that produced in the dynamical ejecta. Due to its moderately high entropy, disk outflows contain a small residual fraction ~1% of helium, which could produce a unique spectroscopic signature.

  17. Massive Black Hole Binary Inspirals: Results from the LISA Parameter Estimation Taskforce

    E-Print Network [OSTI]

    K. G. Arun; Stas Babak; Emanuele Berti; Neil Cornish; Curt Cutler; Jonathan Gair; Scott A. Hughes; Bala R. Iyer; Ryan N. Lang; Ilya Mandel; Edward K. Porter; Bangalore S. Sathyaprakash; Siddhartha Sinha; Alicia M. Sintes; Miquel Trias; Chris Van Den Broeck; Marta Volonteri

    2009-03-30T23:59:59.000Z

    The LISA Parameter Estimation (LISAPE) Taskforce was formed in September 2007 to provide the LISA Project with vetted codes, source distribution models, and results related to parameter estimation. The Taskforce's goal is to be able to quickly calculate the impact of any mission design changes on LISA's science capabilities, based on reasonable estimates of the distribution of astrophysical sources in the universe. This paper describes our Taskforce's work on massive black-hole binaries (MBHBs). Given present uncertainties in the formation history of MBHBs, we adopt four different population models, based on (i) whether the initial black-hole seeds are small or large, and (ii) whether accretion is efficient or inefficient at spinning up the holes. We compare four largely independent codes for calculating LISA's parameter-estimation capabilities. All codes are based on the Fisher-matrix approximation, but in the past they used somewhat different signal models, source parametrizations and noise curves. We show that once these differences are removed, the four codes give results in extremely close agreement with each other. Using a code that includes both spin precession and higher harmonics in the gravitational-wave signal, we carry out Monte Carlo simulations and determine the number of events that can be detected and accurately localized in our four population models.

  18. Long-term evolution of double white dwarf binaries accreting through direct impact

    E-Print Network [OSTI]

    Kremer, Kyle; Kalogera, Vassiliki

    2015-01-01T23:59:59.000Z

    We calculate the long-term evolution of angular momentum in double white dwarf binaries undergoing direct impact accretion over a broad range of parameter space. We allow the rotation rate of both components to vary, and account for the exchange of angular momentum between the spins of the white dwarfs and the orbit, while conserving the total angular momentum. We include gravitational, tidal, and mass transfer effects in the orbital evolution, and allow the Roche radius of the donor star to vary with both the stellar mass and the rotation rate. We examine the long-term stability of these systems, focusing in particular on those systems that may be progenitors of AM CVn or Type Ia Supernovae. We find that our analysis yields an increase in the predicted number of stable systems compared to that in previous studies. Additionally, we find that by properly accounting for the effects of asynchronism between the donor and the orbit on the Roche-lobe size, we eliminate oscillations in the orbital parameters which a...

  19. On Normal Numbers Veronica Becher

    E-Print Network [OSTI]

    Figueira, Santiago

    ends with all zeros; hence, q is not simply normal to base b. 3/23 #12;The problem is still open Theorem (Borel 1909) Almost all real numbers are absolutely normal. Problem (Borel 1909) Give an example transducers. Huffman 1959 calls them lossless compressors. A direct proof of the above theorem Becher

  20. Brookhaven National Laboratory Number: Revision

    E-Print Network [OSTI]

    Ohta, Shigemi

    NATIONAL LABORATORY LASER CONTROLLED AREA STANDARD OPERATING PROCEDURE (SOP) This document defines OPERATIONS Operation Maintenance Service Specific Operation (specify) #12;Number: PS-ESH-0083 Revision: 01 the safety management program for the laser system(s) listed below. All American National Standard Institute

  1. Statistical physics of a model binary genetic switch with linear feedback

    E-Print Network [OSTI]

    Paolo Visco; Rosalind J. Allen; Martin R. Evans

    2009-03-31T23:59:59.000Z

    We study the statistical properties of a simple genetic regulatory network that provides heterogeneity within a population of cells. This network consists of a binary genetic switch in which stochastic flipping between the two switch states is mediated by a "flipping" enzyme. Feedback between the switch state and the flipping rate is provided by a linear feedback mechanism: the flipping enzyme is only produced in the on switch state and the switching rate depends linearly on the copy number of the enzyme. This work generalises the model of [Phys. Rev. Lett., 101, 118104] to a broader class of linear feedback systems. We present a complete analytical solution for the steady-state statistics of the number of enzyme molecules in the on and off states, for the general case where the enzyme can mediate flipping in either direction. For this general case we also solve for the flip time distribution, making a connection to first passage and persistence problems in statistical physics. We show that the statistics of the model are non-Poissonian, leading to a peak in the flip time distribution. The occurrence of such a peak is analysed as a function of the parameter space. We present a new relation between the flip time distributions measured for two relevant choices of initial condition. We also introduce a new correlation measure to show that this model can exhibit long-lived temporal correlations, thus providing a primitive form of cellular memory. Motivated by DNA replication as well as by evolutionary mechanisms involving gene duplication, we study the case of two switches in the same cell. This results in correlations between the two switches; these can either positive or negative depending on the parameter regime.

  2. Binary Black Holes in Quasi-Stationary Circular Orbits

    E-Print Network [OSTI]

    Brian D. Baker

    2002-05-18T23:59:59.000Z

    We propose a method of determining solutions to the constraint equations of General Relativity approximately describing binary black holes in quasi-stationary circular orbits. Black holes with arbitrary linear momenta are constructed in the manner suggested by Brandt and Brugmann. The quasi-stationary circular orbits are determined by local minima in the ADM mass in a manner similar to Baumgarte and Cook; however, rather than fixing the area of the apparent horizon, we fix the value of the bare masses of the holes. We numerically generate an evolutionary sequence of quasi-stationary circular orbits up to and including the innermost stable circular orbit. We compare our results with post-Newtonian expectations as well as the results of Cook and Baumgarte. We also generate additional numerical results describing the dynamics of the geometry due to the emission of gravitational radiation.

  3. Stability of prograde and retrograde planets in circular binary systems

    E-Print Network [OSTI]

    M. H. M. Morais; C. A. Giuppone

    2012-06-22T23:59:59.000Z

    We investigate the stability of prograde versus retrograde planets in circular binary systems using numerical simulations. We show that retrograde planets are stable up to distances closer to the perturber than prograde planets. We develop an analytical model to compute the prograde and retrograde mean motion resonances' locations and separatrices. We show that instability is due to single resonance forcing, or caused by nearby resonances' overlap. We validate our results regarding the role of single resonances and resonances' overlap on orbit stability, by computing surfaces of section of the CR3BP. We conclude that the observed enhanced stability of retrograde planets with respect to prograde planets is due to essential differences between the phase-space topology of retrograde versus prograde resonances (at p/q mean motion ratio, prograde resonance is of order p - q while retrograde resonance is of order p + q).

  4. Low velocity ion stopping in binary ionic mixtures

    SciTech Connect (OSTI)

    Tashev, Bekbolat; Baimbetov, Fazylkhan [Department of Physics, Kazakh National University, Tole Bi 96, Almaty 480012 (Kazakhstan); Deutsch, Claude [LPGP (UMR-CNRS 8578), Universite Paris XI, 91405 Orsay (France); Fromy, Patrice [Direction de l'Informatique, Universite Paris XI, 91405 Orsay (France)

    2008-10-15T23:59:59.000Z

    Attention is focused on the low ion velocity stopping mechanisms in multicomponent and dense target plasmas built of quasiclassical electron fluids neutralizing binary ionic mixtures, such as, deuterium-tritium of current fusion interest, proton-heliumlike iron in the solar interior or proton-helium ions considered in planetology, as well as other mixtures of fiducial concern in the heavy ion beam production of warm dense matter at Bragg peak conditions. The target plasma is taken in a multicomponent dielectric formulation a la Fried-Conte. The occurrence of projectile ion velocities (so-called critical) for which target electron slowing down equals that of given target ion components is also considered. The corresponding multiquadrature computations, albeit rather heavy, can be monitored analytical through a very compact code operating a PC cluster. Slowing down results are systematically scanned with respect to target temperature and electron density, as well as ion composition.

  5. The chromospherically active binary star EI Eridani I. Absolute dimensions

    E-Print Network [OSTI]

    A. Washuettl; K. G. Strassmeier; T. Granzer; M. Weber; K. Oláh

    2008-09-04T23:59:59.000Z

    We present a detailed determination of the astrophysical parameters of the chromospherically active binary star EI Eridani. Our new radial velocities allow to improve the set of orbital elements and reveal long-term variations of the barycentric velocity. A possible third-body orbit with a period of approximately 19 years is presented. Absolute parameters are determined in combination with the Hipparcos parallax. EI Eri's inclination angle of the rotational axis is confined to 56.0 plus/minus 4.5 degrees, its luminosity class IV is confirmed by its radius of 2.37 plus/minus 0.12 R_Sun. A comparison to theoretical stellar evolutionary tracks suggests a mass of 1.09 plus/minus 0.05 M_Sun and an age of approximately 6.15 Gyr. The present investigation is the basis of our long-term Doppler imaging study of its stellar surface.

  6. Heating mechanism affects equipartition in a binary granular system

    E-Print Network [OSTI]

    Hong-Qiang Wang; Narayanan Menon

    2008-03-08T23:59:59.000Z

    Two species of particles in a binary granular system typically do not have the same mean kinetic energy, in contrast to the equipartition of energy required in equilibrium. We investigate the role of the heating mechanism in determining the extent of this non-equipartition of kinetic energy. In most experiments, different species of particle are unequally heated at the boundaries. We show by event-driven simulations that this differential heating at the boundary influences the level of non-equipartition even in the bulk of the system. This conclusion is fortified by studying a numerical model and a solvable stochastic model without spatial degrees of freedom. In both cases, even in the limit where heating events are rare compared to collisions, the effect of the heating mechanism persists.

  7. AA Dor - An Eclipsing sdOB - Brown Dwarf Binary

    E-Print Network [OSTI]

    Thomas Rauch

    2003-11-25T23:59:59.000Z

    AA Dor is an eclipsing, close, post common-envelope binary consisting of a sdOB primary star and an unseen secondary with an extraordinary small mass - formally a brown dwarf. The brown dwarf may have been a former planet which survived a common envelope phase and has even gained mass. A recent determination of the components' masses from results of NLTE spectral analysis and subsequent comparison to evolutionary tracks shows a discrepancy to masses derived from radial-velocity and the eclipse curves. Phase-resolved high-resolution and high-SN spectroscopy was carried out in order to investigate on this problem. We present results of a NLTE spectral analysis of the primary, an analysis of its orbital parameters, and discuss possible evolutionary scenarios.

  8. Beowawe Bottoming Binary Unit - Final Technical Report for EE0002856

    SciTech Connect (OSTI)

    McDonald, Dale Edward

    2013-02-12T23:59:59.000Z

    This binary plant is the first high-output refrigeration based waste heat recovery cycle in the industry. Its working fluid is environmentally friendly and as such, the permits that would be required with a butane based cycle are not necessary. The unit is modularized, meaning that the unit’s individual skids were assembled in another location and were shipped via truck to the plant site. This project proves the technical feasibility of using low temperature brine The development of the unit led to the realization of low temperature, high output, and environmentally friendly heat recovery systems through domestic research and engineering. The project generates additional renewable energy for Nevada, resulting in cleaner air and reduced carbon dioxide emissions. Royalty and tax payments to governmental agencies will increase, resulting in reduced financial pressure on local entities. The major components of the unit were sourced from American companies, resulting in increased economic activity throughout the country.

  9. Optimal Designs for 2^k Factorial Experiments with Binary Response

    E-Print Network [OSTI]

    Yang, Jie; Majumdar, Dibyen

    2011-01-01T23:59:59.000Z

    We consider the problem of obtaining locally D-optimal designs for factorial experiments with binary response and $k$ qualitative factors at two levels each. Yang, Mandal and Majumdar (2011) considered this problem for $2^2$ factorial experiments. In this paper, we generalize the results for $2^k$ designs and explore in new directions. We obtain a characterization for a design to be locally D-optimal. Based on this characterization, we develop efficient numerical techniques to search for locally D-optimal designs. We also investigate the properties of fractional factorial designs and study the robustness of locally D-optimal designs. Using prior distribution on the parameters, we investigate EW D-optimal designs, that are designs which maximize the determinant of the expected information matrix. It turns out that these designs are much easier to find and still highly efficient compared to Bayesian D-optimal designs, as well as quite robust.

  10. Absolute properties of the eclipsing binary star IM Persei

    SciTech Connect (OSTI)

    Lacy, Claud H. Sandberg [Physics Department, University of Arkansas, Fayetteville, AR 72701 (United States); Torres, Guillermo [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Fekel, Francis C.; Muterspaugh, Matthew W. [Center of Excellence in Information Systems, Tennessee State University, Nashville, TN 37209 (United States); Southworth, John, E-mail: clacy@uark.edu, E-mail: gtorres@cfa.harvard.edu, E-mail: fekel@evans.tsuniv.edu, E-mail: matthew1@coe.tsuniv.edu, E-mail: astro.js@keele.ac.uk [Astrophysics Group, Keele University, Staffordshire, ST5 5BG (United Kingdom)

    2015-01-01T23:59:59.000Z

    IM Per is a detached A7 eccentric eclipsing binary star. We have obtained extensive measurements of the light curve (28,225 differential magnitude observations) and radial velocity curve (81 spectroscopic observations) which allow us to fit orbits and determine the absolute properties of the components very accurately: masses of 1.7831 ± 0.0094 and 1.7741 ± 0.0097 solar masses, and radii of 2.409 ± 0.018 and 2.366 ± 0.017 solar radii. The orbital period is 2.25422694(15) days and the eccentricity is 0.0473(26). A faint third component was detected in the analysis of the light curves, and also directly observed in the spectra. The observed rate of apsidal motion is consistent with theory (U = 151.4 ± 8.4 year). We determine a distance to the system of 566 ± 46 pc.

  11. The precession of eccentric discs in close binaries

    E-Print Network [OSTI]

    James R. Murray

    1999-11-25T23:59:59.000Z

    We consider the precession rates of eccentric discs in close binaries, and compare theoretical predictions with the results of numerical disc simulations and with observed superhump periods. A simple dynamical model for precession is found to be inadequate. For mass ratios less than approximately 1/4 a linear dynamical model does provide an upper limit for disc precession rates. Theory suggests that pressure forces have a significant retrograde impact upon the precession rate (Lubow 1992). We find that the disc precession rates for three systems with accurately known mass ratios are significantly slower than predicted by the dynamical theory, and we attribute the difference to pressure forces. By assuming that pressure forces of similar magnitude occur in all superhumping systems, we obtain an improved fit to superhump observations.

  12. Maine Natural Gas Number of Commercial Consumers (Number of Elements)

    Gasoline and Diesel Fuel Update (EIA)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645 3,625 1,006 492 742 33 111 1,613 122 40 Buildingto China (Million Cubic Feet) 3 0 07,755,432Commercial Consumers (Number

  13. Minnesota Natural Gas Number of Commercial Consumers (Number of Elements)

    Gasoline and Diesel Fuel Update (EIA)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645 3,625 1,006 492 742 33 111 1,613 122 40 Buildingto China (Million Cubic Feet)Commercial Consumers (Number of Elements)

  14. Minnesota Natural Gas Number of Industrial Consumers (Number of Elements)

    Gasoline and Diesel Fuel Update (EIA)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645 3,625 1,006 492 742 33 111 1,613 122 40 Buildingto China (Million Cubic Feet)Commercial Consumers (Number of

  15. Kansas Natural Gas Number of Residential Consumers (Number of Elements)

    Annual Energy Outlook 2013 [U.S. Energy Information Administration (EIA)]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645 3,625 1,006 492 742 33 111 1,613 122 40Coal Stocks at1,066,688ElectricityLessAprilResidential Consumers (Number of

  16. Tennessee Natural Gas Number of Residential Consumers (Number of Elements)

    U.S. Energy Information Administration (EIA) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5 Tables July 1996 Energy Information Administration Office ofthroughYear Jan FebDecadeDecade217523,552.1Residential Consumers (Number

  17. Wisconsin Natural Gas Number of Residential Consumers (Number of Elements)

    U.S. Energy Information Administration (EIA) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5 Tables July 1996 Energy Information Administration Office ofthroughYear JanYearFuel5,266 6,090Industrial Consumers (Number

  18. Vermont Natural Gas Number of Commercial Consumers (Number of Elements)

    Gasoline and Diesel Fuel Update (EIA)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645 3,625 1,006 492 742 33 111 1,613 122 40 Buildingto17 34 44Year Jan FebIncreasesCommercial Consumers (Number of Elements)

  19. Vermont Natural Gas Number of Industrial Consumers (Number of Elements)

    Gasoline and Diesel Fuel Update (EIA)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645 3,625 1,006 492 742 33 111 1,613 122 40 Buildingto17 34 44Year Jan FebIncreasesCommercial Consumers (Number of

  20. Georgia Natural Gas Number of Industrial Consumers (Number of Elements)

    Annual Energy Outlook 2013 [U.S. Energy Information Administration (EIA)]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645 3,625 1,006 492 742 33 111 1,613 122 40CoalLease(Billion2,12803 Table A1.GasYear JanPriceIndustrial Consumers (Number of

  1. Isothermal vapor-liquid equilibria for benzene + cyclohexane + 1-propanol and for three constituent binary systems

    SciTech Connect (OSTI)

    Kurihara, Kiyofumi; Uchiyama, Masanori; Kojima, Kazuo [Nihon Univ., Tokyo (Japan). Dept. of Industrial Chemistry] [Nihon Univ., Tokyo (Japan). Dept. of Industrial Chemistry

    1997-01-01T23:59:59.000Z

    Isothermal vapor-liquid equilibria were measured for the ternary system of benzene + cyclohexane + 1-propanol and its constituent binary systems of benzene + cyclohexane, cyclohexane + 1-propanol, and benzene + 1-propanol at 323.15 and 333.15 K, using the apparatus proposed in a previous study. The experimental binary data were correlated using the NRTL equation. The ternary system was predicted using the binary NRTL parameters. The average absolute percent deviations between the predicted and experimental ternary total pressures are 0.5% at 323.15 K and 0.4% at 333.15 K.

  2. Properties and nature of Be stars 30. Reliable physical properties of a semi-detached B9.5e+G8III binary BR CMi = HD 61273 compared to those of other well studied semi-detached emission-line binaries

    E-Print Network [OSTI]

    Harmanec, P; Nemravová, J A; Royer, F; Briot, D; North, P; Lampens, P; Frémat, Y; Yang, S; Boži?, H; Kotková, L; Škoda, P; Šlechta, M; Kor?áková, D; Wolf, M; Zasche, P

    2014-01-01T23:59:59.000Z

    Reliable determination of the basic physical properties of hot emission-line binaries with Roche-lobe filling secondaries is important for developing the theory of mass exchange in binaries. It is a very hard task, however, which is complicated by the presence of circumstellar matter in these systems. So far, only a small number of systems with accurate values of component masses, radii, and other properties are known. Here, we report the first detailed study of a new representative of this class of binaries, BR CMi, based on the analysis of radial velocities and multichannel photometry from several observatories, and compare its physical properties with those for other well-studied systems. BR CMi is an ellipsoidal variable seen under an intermediate orbital inclination of ~51 degrees, and it has an orbital period of 12.919059(15) d and a circular orbit. We used the disentangled component spectra to estimate the effective temperatures 9500(200) K and 4655(50) K by comparing them with model spectra. They corr...

  3. TIGER: A data analysis pipeline for testing the strong-field dynamics of general relativity with gravitational wave signals from coalescing compact binaries

    E-Print Network [OSTI]

    Michalis Agathos; Walter Del Pozzo; Tjonnie G. F. Li; Chris Van Den Broeck; John Veitch; Salvatore Vitale

    2014-06-06T23:59:59.000Z

    The direct detection of gravitational waves with upcoming second-generation gravitational wave detectors such as Advanced LIGO and Virgo will allow us to probe the genuinely strong-field dynamics of general relativity (GR) for the first time. We present a data analysis pipeline called TIGER (Test Infrastructure for GEneral Relativity), which is designed to utilize detections of compact binary coalescences to test GR in this regime. TIGER is a model-independent test of GR itself, in that it is not necessary to compare with any specific alternative theory. It performs Bayesian inference on two hypotheses: the GR hypothesis $\\mathcal{H}_{\\rm GR}$, and $\\mathcal{H}_{\\rm modGR}$, which states that one or more of the post-Newtonian coefficients in the waveform are not as predicted by GR. By the use of multiple sub-hypotheses of $\\mathcal{H}_{\\rm modGR}$, in each of which a different number of parameterized deformations of the GR phase are allowed, an arbitrarily large number of 'testing parameters' can be used without having to worry about a model being insufficiently parsimonious if the true number of extra parameters is in fact small. TIGER is well-suited to the regime where most sources have low signal-to-noise ratios, again through the use of these sub-hypotheses. Information from multiple sources can trivially be combined, leading to a stronger test. We focus on binary neutron star coalescences, for which sufficiently accurate waveform models are available that can be generated fast enough on a computer to be fit for use in Bayesian inference. We show that the pipeline is robust against a number of fundamental, astrophysical, and instrumental effects, such as differences between waveform approximants, a limited number of post-Newtonian phase contributions being known, the effects of neutron star spins and tidal deformability on the orbital motion, and instrumental calibration errors.

  4. Particle Number & Particulate Mass Emissions Measurements on...

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    Number & Particulate Mass Emissions Measurements on a 'Euro VI' Heavy-duty Engine using the PMP Methodologies Particle Number & Particulate Mass Emissions Measurements on a 'Euro...

  5. Transformations in Massive Binary Stars: CRA Colloquium, Jan. 15, 2009 1 Mass and Angular Momentum

    E-Print Network [OSTI]

    Gies, Douglas R.

    over lives Progenitors of the Long Gamma Ray Bursts Binary Star Surveys Early Stages of Interacting, 2009 3 Progenitors of Long Gamma Ray Bursts Collapsar model (Woosley 1993): core of a massive, fast

  6. Linking electromagnetic and gravitational radiation in coalescing binary neutron stars Carlos Palenzuela1

    E-Print Network [OSTI]

    Lumsdaine, Andrew

    a fundamental role in the production of gamma ray bursts. These compact binary systems are also among the most model of short, hard gamma ray bursts (SGRBs) (see e.g. [2] for a review). This model envisions

  7. THE YOUNGEST KNOWN X-RAY BINARY: CIRCINUS X-1 AND ITS NATAL SUPERNOVA REMNANT

    E-Print Network [OSTI]

    Heinz, S.

    Because supernova remnants are short-lived, studies of neutron star X-ray binaries within supernova remnants probe the earliest stages in the life of accreting neutron stars. However, such objects are exceedingly rare: ...

  8. X-ray spectroscopy of neutron star low-mass X-ray binaries

    E-Print Network [OSTI]

    Krauss, Miriam Ilana

    2007-01-01T23:59:59.000Z

    In this thesis, I present work spanning a variety of topics relating to neutron star lowmass X-ray binaries (LMXBs) and utilize spectral information from X-ray observations to further our understanding of these sources. ...

  9. High speed simulation of microprocessor systems using LTU dynamic binary translation 

    E-Print Network [OSTI]

    Jones, Daniel

    2010-01-01T23:59:59.000Z

    This thesis presents new simulation techniques designed to speed up the simulation of microprocessor systems. The advanced simulation techniques may be applied to the simulator class which employs dynamic binary translation ...

  10. Radial Velocity Curves of Ellipsoidal Red Giant Binaries in the Large Magellanic Cloud

    E-Print Network [OSTI]

    Nie, J D

    2015-01-01T23:59:59.000Z

    Ellipsoidal red giant binaries are close binary systems where an unseen, relatively close companion distorts the red giant, leading to light variations as the red giant moves around its orbit. These binaries are likely to be the immediate evolutionary precursors of close binary planetary nebula and post-asymptotic giant branch and post-red giant branch stars. Due to the MACHO and OGLE photometric monitoring projects, the light variability nature of these ellipsoidal variables has been well studied. However, due to the lack of radial velocity curves, the nature of their masses, separations, and other orbital details has so far remained largely unknown. In order to improve this situation, we have carried out spectral monitoring observations of a large sample of 80 ellipsoidal variables in the Large Magellanic Cloud and we have derived radial velocity curves. At least 12 radial velocity points with good quality were obtained for most of the ellipsoidal variables. The radial velocity data are provided with this p...

  11. Observational and evolutionary studies of neutron star X-ray binaries

    E-Print Network [OSTI]

    Lin, Jinrong, Ph. D. Massachusetts Institute of Technology

    2011-01-01T23:59:59.000Z

    In this thesis, we present our observational and evolutionary studies of neutron stars in X-ray binary systems. A variety of topics are discussed, which are all related by a single scientific theme, namely, helping to set ...

  12. Construction and characterization of a peach binary bacterial artificial chromosome library

    E-Print Network [OSTI]

    Wakefield, Laura

    2002-01-01T23:59:59.000Z

    Peach [Prunus persica (L.) Batch] has been proposed as a model organism for woody perennials. To facilitate genomic research in peach, a binary bacterial artificial chromosome (BIBAC) library of var. Texking was constructed using a plant...

  13. Search for gravitational waves from binary black hole inspiral, merger and ringdown

    E-Print Network [OSTI]

    The LIGO Scientific Collaboration; the Virgo Collaboration; J. Abadie; B. P. Abbott; R. Abbott; M. Abernathy; T. Accadia; F. Acernese; C. Adams; R. Adhikari; P. Ajith; B. Allen; G. S. Allen; E. Amador Ceron; R. S. Amin; S. B. Anderson; W. G. Anderson; F. Antonucci; M. A. Arain; M. C. Araya; M. Aronsson; Y. Aso; S. M. Aston; P. Astone; D. Atkinson; P. Aufmuth; C. Aulbert; S. Babak; P. Baker; G. Ballardin; T. Ballinger; S. Ballmer; D. Barker; S. Barnum; F. Barone; B. Barr; P. Barriga; L. Barsotti; M. Barsuglia; M. A. Barton; I. Bartos; R. Bassiri; M. Bastarrika; J. Bauchrowitz; Th. S. Bauer; B. Behnke; M. G. Beker; A. Belletoile; M. Benacquista; A. Bertolini; J. Betzwieser; N. Beveridge; P. T. Beyersdorf; I. A. Bilenko; G. Billingsley; J. Birch; S. Birindelli; R. Biswas; M. Bitossi; M. A. Bizouard; E. Black; J. K. Blackburn; L. Blackburn; D. Blair; B. Bland; M. Blom; C. Boccara; O. Bock; T. P. Bodiya; R. Bondarescu; F. Bondu; L. Bonelli; R. Bonnand; R. Bork; M. Born; V. Boschi; S. Bose; L. Bosi; B. Bouhou; M. Boyle; S. Braccini; C. Bradaschia; P. R. Brady; V. B. Braginsky; J. E. Brau; J. Breyer; D. O. Bridges; A. Brillet; M. Brinkmann; V. Brisson; M. Britzger; A. F. Brooks; D. A. Brown; R. Budzy?ski; T. Bulik; H. J. Bulten; A. Buonanno; J. Burguet-Castell; O. Burmeister; D. Buskulic; C. Buy; R. L. Byer; L. Cadonati; G. Cagnoli; J. Cain; E. Calloni; J. B. Camp; E. Campagna; P. Campsie; J. Cannizzo; K. Cannon; B. Canuel; J. Cao; C. Capano; F. Carbognani; S. Caride; S. Caudill; M. Cavaglia`; F. Cavalier; R. Cavalieri; G. Cella; C. Cepeda; E. Cesarini; O. Chaibi; T. Chalermsongsak; E. Chalkley; P. Charlton; E. Chassande-Mottin; S. Chelkowski; Y. Chen; A. Chincarini; N. Christensen; S. S. Y. Chua; C. T. Y. Chung; D. Clark; J. Clark; J. H. Clayton; F. Cleva; E. Coccia; C. N. Colacino; J. Colas; A. Colla; M. Colombini; R. Conte; D. Cook; T. R. Corbitt; N. Cornish; A. Corsi; C. A. Costa; J. -P. Coulon; D. M. Coward; D. C. Coyne; J. D. E. Creighton; T. D. Creighton; A. M. Cruise; R. M. Culter; A. Cumming; L. Cunningham; E. Cuoco; K. Dahl; S. L. Danilishin; R. Dannenberg; S. D'Antonio; K. Danzmann; K. Das; V. Dattilo; B. Daudert; M. Davier; G. Davies; A. Davis; E. J. Daw; R. Day; T. Dayanga; R. De Rosa; D. DeBra; G. Debreczeni; J. Degallaix; M. del Prete; V. Dergachev; R. DeRosa; R. DeSalvo; P. Devanka; S. Dhurandhar; L. Di Fiore; A. Di Lieto; I. Di Palma; M. Di Paolo Emilio; A. Di Virgilio; M. Díaz; A. Dietz; F. Donovan; K. L. Dooley; E. E. Doomes; S. Dorsher; E. S. D. Douglas; M. Drago; R. W. P. Drever; J. C. Driggers; J. Dueck; J. -C. Dumas; T. Eberle; M. Edgar; M. Edwards; A. Effler; P. Ehrens; G. Ely; R. Engel; T. Etzel; M. Evans; T. Evans; V. Fafone; S. Fairhurst; Y. Fan; B. F. Farr; D. Fazi; H. Fehrmann; D. Feldbaum; I. Ferrante; F. Fidecaro; L. S. Finn; I. Fiori; R. Flaminio; M. Flanigan; K. Flasch; S. Foley; C. Forrest; E. Forsi; L. A. Forte; N. Fotopoulos; J. -D. Fournier; J. Franc; S. Frasca; F. Frasconi; M. Frede; M. Frei; Z. Frei; A. Freise; R. Frey; T. T. Fricke; D. Friedrich; P. Fritschel; V. V. Frolov; P. Fulda; M. Fyffe; M. Galimberti; L. Gammaitoni; J. A. Garofoli; F. Garufi; M. E. Gáspár; G. Gemme; E. Genin; A. Gennai; I. Gholami; S. Ghosh; J. A. Giaime; S. Giampanis; K. D. Giardina; A. Giazotto; C. Gill; E. Goetz; L. M. Goggin; G. González; M. L. Gorodetsky; S. Goßler; R. Gouaty; C. Graef; M. Granata; A. Grant; S. Gras; C. Gray; R. J. S. Greenhalgh; A. M. Gretarsson; C. Greverie; R. Grosso; H. Grote; S. Grunewald; G. M. Guidi; E. K. Gustafson; R. Gustafson; B. Hage; P. Hall; J. M. Hallam; D. Hammer; G. Hammond; J. Hanks; C. Hanna; J. Hanson; J. Harms; G. M. Harry; I. W. Harry; E. D. Harstad; K. Haughian; K. Hayama; J. -F. Hayau; T. Hayler; J. Heefner; H. Heitmann; P. Hello; I. S. Heng; A. W. Heptonstall; M. Hewitson; S. Hild; E. Hirose; D. Hoak; K. A. Hodge; K. Holt; D. J. Hosken; J. Hough; E. J. Howell; D. Hoyland; D. Huet; B. Hughey; S. Husa; S. H. Huttner; T. Huynh-Dinh; D. R. Ingram; R. Inta; T. Isogai; A. Ivanov; P. Jaranowski; W. W. Johnson; D. I. Jones; G. Jones; R. Jones; L. Ju; P. Kalmus; V. Kalogera; S. Kandhasamy; J. B. Kanner; E. Katsavounidis; K. Kawabe; S. Kawamura; F. Kawazoe; W. Kells; D. G. Keppel; A. Khalaidovski; F. Y. Khalili; E. A. Khazanov; H. Kim; P. J. King; D. L. Kinzel; J. S. Kissel; S. Klimenko; V. Kondrashov; R. Kopparapu; S. Koranda; I. Kowalska; D. Kozak; T. Krause; V. Kringel; S. Krishnamurthy; B. Krishnan; A. Królak; G. Kuehn; J. Kullman; R. Kumar; P. Kwee; M. Landry; M. Lang; B. Lantz; N. Lastzka; A. Lazzarini; P. Leaci; J. Leong; I. Leonor; N. Leroy; N. Letendre; J. Li; T. G. F. Li; N. Liguori; H. Lin; P. E. Lindquist; N. A. Lockerbie; D. Lodhia; M. Lorenzini; V. Loriette; M. Lormand; G. Losurdo; P. Lu; J. Luan; M. Lubinski; A. Lucianetti; H. Lück; A. D. Lundgren; B. Machenschalk; M. MacInnis; M. Mageswaran; K. Mailand; E. Majorana

    2011-02-18T23:59:59.000Z

    We present the first modeled search for gravitational waves using the complete binary black hole gravitational waveform from inspiral through the merger and ringdown for binaries with negligible component spin. We searched approximately 2 years of LIGO data taken between November 2005 and September 2007 for systems with component masses of 1-99 solar masses and total masses of 25-100 solar masses. We did not detect any plausible gravitational-wave signals but we do place upper limits on the merger rate of binary black holes as a function of the component masses in this range. We constrain the rate of mergers for binary black hole systems with component masses between 19 and 28 solar masses and negligible spin to be no more than 2.0 per Mpc^3 per Myr at 90% confidence.

  14. On the Kinematics of Solar Mirrors Using Massively Parallel Binary Actuation

    E-Print Network [OSTI]

    Dubowsky, Steven

    Precision mirrors are required for effective solar energy collectors. Manufacturing such mirrors and making them robust to disturbances such as thermal gradients is expensive. In this paper, the use of parallel binary ...

  15. Adsorption and desorption of binary mixtures of volatile organic contaminants on soil

    E-Print Network [OSTI]

    Guo, Yang

    1995-01-01T23:59:59.000Z

    , the potential theory and the ideal adsorbed solution theory for mixture adsorption were also evaluated for prediction of the experimental results for binary adsorption. All models failed for prediction of the BET type III isotherms when methanol was present...

  16. Synthesis and characterization of patterned surfaces and catalytically relevant binary nanocrystalline intermetallic compounds 

    E-Print Network [OSTI]

    Cable, Robert E.

    2009-05-15T23:59:59.000Z

    -metallics are not yet matured. In response to this deficiency, we have developed several solution-based methods to synthesize nanocrystalline binary alloy and intermetallic compounds. This dissertation describes the processes we have developed, as well as our...

  17. Synthesis and characterization of patterned surfaces and catalytically relevant binary nanocrystalline intermetallic compounds 

    E-Print Network [OSTI]

    Cable, Robert E.

    2008-10-10T23:59:59.000Z

    -metallics are not yet matured. In response to this deficiency, we have developed several solution-based methods to synthesize nanocrystalline binary alloy and intermetallic compounds. This dissertation describes the processes we have developed, as well as our...

  18. On the rarity of x-ray binaries with Wolf-Rayet donors

    DOE Public Access Gateway for Energy & Science Beta (PAGES Beta)

    Linden, T; Valsecchi, F; Kalogera, V

    2012-03-06T23:59:59.000Z

    The paucity of High mass X-Ray binaries (HMXB) consisting of a neutron star (NS) accretor and Wolf-Rayet (WR) donor has long been at odds with expectations from population synthesis studies indicating that these systems should survive as the evolved offspring of the observed HMXB population. This tension is particularly troubling in light of recent observations uncovering a preponderance of HMXBs containing loosely bound Be donors which would be expected to naturally evolve into WR-HMXBs. Reconciling the unexpectedly large population of Be-HMXBs with the lack of observed WR-HMXB sources thus serves to isolate the dynamics of CE physics from other binary evolution parameters. Here, we find that binary mergers during CE events must be common in order to resolve tension between these observed populations. Furthermore, future observations which better constrain the background population of loosely bound O/B-NS binaries are likely to place significant constraints on the efficiency of CE removal.

  19. accreting low-mass binary: Topics by E-print Network

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    in post-accretion Low-Mass X-ray Binaries: A universal model for short-hard Gamma-Ray Bursts CERN Preprints Summary: We show that several features reminiscent of short-hard...

  20. adc x-ray binary: Topics by E-print Network

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    systems. Sudip Bhattacharyya 2010-02-24 17 X-ray Transients from X-ray Binaries to Gamma Ray Bursts CERN Preprints Summary: We discuss three classes of x-ray transients to...

  1. Parameter estimation for compact binary coalescence signals with the first generation gravitational-wave detector network

    E-Print Network [OSTI]

    Barsotti, Lisa

    Compact binary systems with neutron stars or black holes are one of the most promising sources for ground-based gravitational-wave detectors. Gravitational radiation encodes rich information about source physics; thus ...

  2. RADIAL VELOCITIES OF GALACTIC O-TYPE STARS. II. SINGLE-LINED SPECTROSCOPIC BINARIES

    SciTech Connect (OSTI)

    Williams, S. J.; Gies, D. R. [Center for High Angular Resolution Astronomy and Department of Physics and Astronomy, Georgia State University, P.O. Box 4106, Atlanta, GA 30302-4106 (United States); Hillwig, T. C. [Department of Physics and Astronomy, Valparaiso University, Valparaiso, IN 46383 (United States); McSwain, M. V. [Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015 (United States); Huang, W., E-mail: swilliams@chara.gsu.edu, E-mail: gies@chara.gsu.edu, E-mail: todd.hillwig@valpo.edu, E-mail: mcswain@lehigh.edu, E-mail: hwenjin@astro.washington.edu [Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580 (United States)

    2013-02-01T23:59:59.000Z

    We report on new radial velocity measurements of massive stars that are either suspected binaries or lacking prior observations. This is part of a survey to identify and characterize spectroscopic binaries among O-type stars with the goal of comparing the binary fraction of field and runaway stars with those in clusters and associations. We present orbits for HDE 308813, HD 152147, HD 164536, BD-16 Degree-Sign 4826, and HDE 229232, Galactic O-type stars exhibiting single-lined spectroscopic variation. By fitting model spectra to our observed spectra, we obtain estimates for effective temperature, surface gravity, and rotational velocity. We compute orbital periods and velocity semiamplitudes for each system and note the lack of photometric variation for any system. These binaries probably appear single-lined because the companions are faint and because their orbital Doppler shifts are small compared to the width of the rotationally broadened lines of the primary.

  3. Post-Newtonian Theory for Precision Doppler Measurements of Binary Star Orbits

    E-Print Network [OSTI]

    Kopeikin, S M

    1999-01-01T23:59:59.000Z

    The determination of velocities of stars from precise Doppler measurements is described here using relativistic theory of astronomical reference frames so as to determine the Keplerian and post-Keplerian parameters of binary systems. Seven appropriate reference frames are introduced and then we apply successive Lorentz transformations and the relativistic equation of light propagation to establish the exact treatment of Doppler effect in binary systems, both in special and general relativity theories. As a result, the Doppler shift is a sum of (1) linear in $c^{-1}$ terms, which include the ordinary Doppler effect and its variation due to the secular radial acceleration of the binary with respect to observer; (2) terms proportional to $c^{-2}$, which include the contributions from the quadratic Doppler effect caused by the relative motion of binary star with respect to the Solar system, motion of the particle emitting light and diurnal rotational motion of observer, orbital motion of the star around the binar...

  4. Radial Velocities of Galactic O-Type Stars. II. Single-lined Spectroscopic Binaries

    E-Print Network [OSTI]

    Williams, S J; Hillwig, T C; McSwain, M V; Huang, W

    2012-01-01T23:59:59.000Z

    We report on new radial velocity measurements of massive stars that are either suspected binaries or lacking prior observations. This is part of a survey to identify and characterize spectroscopic binaries among O-type stars with the goal of comparing the binary fraction of field and runaway stars with those in clusters and associations. We present orbits for HDE 308813, HD 152147, HD 164536, BD-16 4826 and HDE 229232, Galactic O-type stars exhibiting single-lined spectroscopic variation. By fitting model spectra to our observed spectra we obtain estimates for effective temperature, surface gravity, and rotational velocity. We compute orbital periods and velocity semiamplitudes for each system and note the lack of photometric variation for any system. These binaries probably appear single-lined because the companions are faint and because their orbital Doppler shifts are small compared to the width of the rotationally broadened lines of the primary.

  5. A Type System for Certified Binaries Zhong Shao Bratin Saha Valery Trifonov Nikolaos Papaspyrou

    E-Print Network [OSTI]

    Trifonov, Valery

    A Type System for Certified Binaries Zhong Shao Bratin Saha Valery Trifonov Nikolaos Papaspyrou Department of Computer Science, Yale University New Haven, CT 06520-8285, U.S.A. {shao, saha, trifonov

  6. Ba and Ni speciation in a nodule of binary Mn oxide phase composition from Lake Baikal

    E-Print Network [OSTI]

    , and absorption spectroscopy. Fe is speciated as goethite, and Mn as romanechite (psilomelane) and 10 A is separated from the other type by goethite. The binary Mn oxide banding pattern is interpreted by a two

  7. A New Method of Accelerated Bayesian Inference for Comparable Mass Binaries in both Ground and Space-Based Gravitational Wave Astronomy

    E-Print Network [OSTI]

    Edward K. Porter

    2014-11-03T23:59:59.000Z

    With the advance in computational resources, Bayesian inference is increasingly becoming the standard tool of practise in GW astronomy. However, algorithms such as Markov Chain Monte Carlo (MCMC) require a large number of iterations to guarantee convergence to the target density. Each chain demands a large number of evaluations of the likelihood function, and in the case of a Hessian MCMC, calculations of the Fisher information matrix for use as a proposal distribution. As each iteration requires the generation of at least one gravitational waveform, we very quickly reach a point of exclusion for current Bayesian algorithms, especially for low mass systems where the length of the waveforms is large and the waveform generation time is on the order of seconds. This suddenly demands a timescale of many weeks for a single MCMC. As each likelihood and Fisher information matrix calculation requires the evaluation of noise-weighted scalar products, we demonstrate that by using the linearity of integration, and the fact that more than 90% of the generation time is spent at frequencies less that one third of the maximum, we can construct composite integrals that speed up the MCMCs for comparable mass binaries by a factor of between 3.5 and 5.5, depending on the waveform length. This method is both source and detector type independent, and can be applied to any waveform that displays significant frequency evolution, such as stellar mass binaries with Advanced LIGO/Virgo, as well as supermassive black holes with eLISA

  8. Binary and ternary gas mixtures for use in glow discharge closing switches

    DOE Patents [OSTI]

    Hunter, Scott R. (Oak Ridge, TN); Christophorou, Loucas G. (Oak Ridge, TN)

    1990-01-01T23:59:59.000Z

    Highly efficient binary and ternary gas mixtures for use in diffuse glow discharge closing switches are disclosed. The binary mixtures are combinations of helium or neon and selected perfluorides. The ternary mixtures are combinations of helium, neon, or argon, a selected perfluoride, and a small amount of gas that exhibits enhanced ionization characteristics. These mixtures are shown to be the optimum choices for use in diffuse glow discharge closing switches by virtue of the combined physio-electric properties of the mixture components.

  9. Post-Newtonian Theory for Precision Doppler Measurements of Binary Star Orbits

    E-Print Network [OSTI]

    S. M. Kopeikin; L. M. Ozernoy

    1999-01-31T23:59:59.000Z

    The determination of velocities of stars from precise Doppler measurements is described here using relativistic theory of astronomical reference frames so as to determine the Keplerian and post-Keplerian parameters of binary systems. We apply successive Lorentz transformations and the relativistic equation of light propagation to establish the exact treatment of Doppler effect in binary systems both in special and general relativity theories. As a result, the Doppler shift is a sum of (1) linear in $c^{-1}$ terms, which include the ordinary Doppler effect and its variation due to the secular radial acceleration of the binary with respect to observer; (2) terms proportional to $c^{-2}$, which include the contributions from the quadratic Doppler effect caused by the relative motion of binary star with respect to the Solar system, motion of the particle emitting light and diurnal rotational motion of observer, orbital motion of the star around the binary's barycenter, and orbital motion of the Earth; and (3) terms proportional to $c^{-2}$, which include the contributions from redshifts due to gravitational fields of the star, star's companion, Galaxy, Solar system, and the Earth. After parameterization of the binary's orbit we find that the presence of periodically changing terms in the Doppler schift enables us disentangling different terms and measuring, along with the well known Keplerian parameters of the binary, four additional post-Keplerian parameters, including the inclination angle of the binary's orbit, $i$. We briefly discuss feasibility of practical implementation of these theoretical results, which crucially depends on further progress in the technique of precision Doppler measurements.

  10. Gravitational Waves from Coalescing Binary Black Holes: Theoretical and Experimental Challenges

    ScienceCinema (OSTI)

    None

    2011-10-06T23:59:59.000Z

    A network of ground-based interferometric gravitational wave detectors (LIGO/VIRGO/GEO/...) is currently taking data near its planned sensitivity. Coalescing black hole binaries are among the most promising, and most exciting, gravitational wave sources for these detectors. The talk will review the theoretical and experimental challenges that must be met in order to successfully detect gravitational waves from coalescing black hole binaries, and to be able to reliably measure the physical parameters of the source (masses, spins, ...).

  11. Random number stride in Monte Carlo calculations

    SciTech Connect (OSTI)

    Hendricks, J.S.

    1990-01-01T23:59:59.000Z

    Monte Carlo radiation transport codes use a sequence of pseudorandom numbers to sample from probability distributions. A common practice is to start each source particle a predetermined number of random numbers up the pseudorandom number sequence. This number of random numbers skipped between each source particles the random number stride, S. Consequently, the jth source particle always starts with the j{center dot}Sth random number providing correlated sampling'' between similar calculations. A new machine-portable random number generator has been written for the Monte Carlo radiation transport code MCNP providing user's control of the random number stride. First the new MCNP random number generator algorithm will be described and then the effects of varying the stride will be presented. 2 refs., 1 fig.

  12. Device Independent Random Number Generation

    E-Print Network [OSTI]

    Mataj Pivoluska; Martin Plesch

    2015-02-23T23:59:59.000Z

    Randomness is an invaluable resource in today's life with a broad use reaching from numerical simulations through randomized algorithms to cryptography. However, on the classical level no true randomness is available and even the use of simple quantum devices in a prepare-measure setting suffers from lack of stability and controllability. This gave rise to a group of quantum protocols that provide randomness certified by classical statistical tests -- Device Independent Quantum Random Number Generators. In this paper we review the most relevant results in this field, which allow the production of almost perfect randomness with help of quantum devices, supplemented with an arbitrary weak source of additional randomness. This is in fact the best one could hope for to achieve, as with no starting randomness (corresponding to no free will in a different concept) even a quantum world would have a fully deterministic description.

  13. Testing eccentricity pumping mechanisms to model eccentric long period sdB binaries with MESA

    E-Print Network [OSTI]

    Vos, Joris; Marchant, Pablo; Van Winckel, Hans

    2015-01-01T23:59:59.000Z

    Hot subdwarf-B stars in long-period binaries are found to be on eccentric orbits, even though current binary-evolution theory predicts those objects to be circularised before the onset of Roche-lobe overflow (RLOF). We aim to find binary-evolution mechanisms that can explain these eccentric long-period orbits, and reproduce the currently observed period-eccentricity diagram. Three different processes are considered; tidally-enhanced wind mass-loss, phase-dependent RLOF on eccentric orbits and the interaction between a circumbinary disk and the binary. The binary module of the stellar-evolution code MESA (Modules for Experiments in Stellar Astrophysics) is extended to include the eccentricity-pumping processes. The effects of different input parameters on the final period and eccentricity of a binary-evolution model are tested with MESA. The end products of models with only tidally-enhanced wind mass-loss can indeed be eccentric, but these models need to lose too much mass, and invariably end up with a helium ...

  14. The detectability of eccentric compact binary coalescences with advanced gravitational-wave detectors

    E-Print Network [OSTI]

    Michael Coughlin; Patrick Meyers; Eric Thrane; Jialun Luo; Nelson Christensen

    2014-12-19T23:59:59.000Z

    Compact binary coalescences are a promising source of gravitational waves for second-generation interferometric gravitational-wave detectors such as advanced LIGO and advanced Virgo. While most binaries are expected to possess circular orbits, some may be eccentric, for example, if they are formed through dynamical capture. Eccentric orbits can create difficulty for matched filtering searches due to the challenges of creating effective template banks to detect these signals. In previous work, we showed how seedless clustering can be used to detect low-mass ($M_\\text{total}\\leq10M_\\odot$) compact binary coalescences for both spinning and eccentric systems, assuming a circular post-Newtonian expansion. Here, we describe a parameterization that is designed to maximize sensitivity to low-eccentricity ($0\\leq\\epsilon\\leq0.6$) systems, derived from the analytic equations. We show that this parameterization provides a robust and computationally efficient method for detecting eccentric low-mass compact binaries. Based on these results, we conclude that advanced detectors will have a chance of detecting eccentric binaries if optimistic models prove true. However, a null observation is unlikely to firmly rule out models of eccentric binary populations.

  15. Caustic Crossing Microlensing Event by Binary MACHOs and Time Scale Bias

    E-Print Network [OSTI]

    Mareki Honma

    1998-11-25T23:59:59.000Z

    Caustic crossing microlensing events provide us a unique opportunity to measure the relative proper motion of the lens to the source, and so those caused by binary MACHOs are of great importance for understanding the structure of the Galactic halo and the nature of MACHOs. The microlensing event 98-SMC-01, occurred in June 1998, is the first event for which the proper motion is ever measured through the caustic crossing, and this event may be caused by binary MACHOs as we argue in this Letter. Motivated by the possible existence of binary MACHOs, we have performed the Monte Carlo simulations of caustic crossing events by binary MACHOs and investigated the properties and detectability of the events. Our calculation shows that typical caustic crossing events have the interval between two caustic crossings ($t_{\\rm cc}$) of about 5 days. We argue that with the current strategy of binary event search the proper motions of these typical events are not measurable because of the short time scale. Therefore the proper motion distribution measured from caustic crossing events suffers significantly from {`}time scale bias{'}, which is a bias toward finding long time scale events and hence slowly moving lenses. We predict there are two times more short time scale events ($t_{\\rm cc}\\le 10$ days) than long time scale events ($t_{\\rm cc}\\ge 10$ days), and propose an hourly monitoring observation instead of the nightly monitoring currently undertaken to detect caustic crossing events by binary MACHOs more efficiently.

  16. A triple origin for the lack of tight coplanar circumbinary planets around short-period binaries

    E-Print Network [OSTI]

    Hamers, Adrian S; Zwart, Simon F Portegies

    2015-01-01T23:59:59.000Z

    Detection of transiting circumbinary planets is more tractable around short-period binaries, however, no such binaries were found with orbits shorter than 7 days. Short-period main sequence binaries have been suggested to form in triple systems, through a combination of secular Kozai-Lidov cycles and tidal friction (KLCTF). Here, we show that coplanar circumbinary transiting planets are unlikely to exist around short-period binaries, due to triple evolution. We use secular analysis, $N$-body simulations and analytic considerations as well as population synthesis models to characterize their overall properties. We find that the existence of a circumbinary planet in a triple is likely to produce one of the following outcomes. (1) Sufficiently massive planets in tight and/or coplanar orbits around the inner binary can partially or completely quench the KL evolution, `shielding' the inner binary from the secular effects of the tertiary, and not allowing the KLCTF process to take place. In this case, the inner bin...

  17. The Low-Mass X-ray Binary-Globular Cluster connection in NGC 4472

    E-Print Network [OSTI]

    Arunav Kundu; Tom Maccarone; Steve Zepf

    2002-06-13T23:59:59.000Z

    We have analyzed the low mass X-ray binary (LMXB) candidates in a Chandra observation of the giant elliptical galaxy NGC 4472. In a region observed by the Hubble Space Telescope, approximately 40% of the bright (L_X >= 10^37 ergs/s) LMXBs are associated with optically identified globular clusters (GC). This is significantly higher than the fraction of bright LMXBs in Galactic GCs and confirms that GCs are the dominant sites of LMXB formation in early type galaxies. The approximately 4% of NGC 4472 GCs hosting bright LMXBs, on the other hand, is remarkably similar to the fraction of GCs with LMXBs in every other galaxy. Although statistical tests suggest that the luminosity of a cluster is an important driver of LMXB formation in GCs, this appears largely to be a consequence of the greater number of stars in bright clusters. The metallicity of GCs is a strong determinant of LMXB specific frequency, with metal-rich clusters about 3 times more likely to host LMXBs than metal-poor ones. There are weaker dependences on the size of a GC and its distance from the center of the galaxy. The X-ray luminosity does not depend significantly on the properties of the host GC. Furthermore, the spatial distribution and X-ray luminosity function of LMXBs within and outside GCs are indistinguishable. The X-ray luminosity function of both GC-LMXBs and non-GC-LMXBs reveal a break at approximately 3x10^38 ergs/s strongly suggesting that the brightest LMXBs are black hole accretors.

  18. The triple binary star EQ Tau with an active component

    SciTech Connect (OSTI)

    Li, K.; Hu, S.-M. [Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Science and School of Space Science and Physics, Shandong University, Weihai, Weihai 264209 (China); Qian, S.-B.; He, J.-J., E-mail: kaili@sdu.edu.cn, E-mail: likai@ynao.ac.cn, E-mail: husm@sdu.edu.cn [Yunnan Observatories, Chinese Academy of Sciences, P.O. Box 110, Kunming 650011 (China)

    2014-05-01T23:59:59.000Z

    New photometric data of EQ Tau observed in 2010 and 2013 are presented. Light curves obtained in 2000 and 2004 by Yuan and Qian and 2001 by Yang and Liu, together with our two newly determined sets of light curves, were analyzed using the Wilson-Devinney code. The five sets of light curves exhibit very obvious variations, implying that the light curves of EQ Tau show a strong O'Connell effect. We found that EQ Tau is an A-type shallow contact binary with a contact degree of f = 11.8%; variable dark spots on the primary component of EQ Tau were also observed. Using 10 new times of minimum light, together with those collected from the literature, the orbital period change of EQ Tau was analyzed. We found that its orbital period includes a secular decrease (dP/dt = –3.63 × 10{sup –8} days yr{sup –1}) and a cyclic oscillation (A {sub 3} = 0.0058 days and P {sub 3} = 22.7 yr). The secular increase of the period can be explained by mass transfer from the more massive component to the less massive one or/and angular momentum loss due to a magnetic stellar wind. The Applegate mechanism cannot explain the cyclic orbital period change. A probable transit-like event was observed in 2010. Therefore, the cyclic orbital period change of EQ Tau may be due to the light time effect of a third body.

  19. Magnetically-induced outflows from binary neutron star merger remnants

    E-Print Network [OSTI]

    Siegel, Daniel M

    2015-01-01T23:59:59.000Z

    Recent observations by the Swift satellite have revealed long-lasting ($\\sim 10^2-10^5\\,\\mathrm{s}$), "plateau-like" X-ray afterglows in the vast majority of short gamma-ray bursts events. This has put forward the idea of a long-lived millisecond magnetar central engine being generated in a binary neutron star (BNS) merger and being responsible for the sustained energy injection over these timescales ("magnetar model"). We elaborate here on recent simulations that investigate the early evolution of such a merger remnant in general-relativistic magnetohydrodynamics. These simulations reveal very different conditions than those usually assumed for dipole spin-down emission in the magnetar model. In particular, the surrounding of the newly formed NS is polluted by baryons due to a dense, highly magnetized and isotropic wind from the stellar surface that is induced by magnetic field amplification in the interior of the star. The timescales and luminosities of this wind are compatible with early X-ray afterglows, ...

  20. Planet formation in post-common-envelope binaries

    E-Print Network [OSTI]

    Schleicher, Dominik; Völschow, Marcel; Banerjee, Robi; Hessman, Frederic V

    2015-01-01T23:59:59.000Z

    To understand the evolution of planetary systems, it is important to investigate planets in highly evolved stellar systems, and to explore the implications of their observed properties with respect to potential formation scenarios. Observations suggest the presence of giant planets in post-common-envelope binaries (PCEBs). A particularly well-studied system with planetary masses of 1.7 M_J and 7.0 M_J is NN Ser. We show here that a pure first-generation scenario where the planets form before the common envelope (CE) phase and the orbits evolve due to the changes in the gravitational potential is inconsistent with the current data. We propose a second-generation scenario where the planets are formed from the material that is ejected during the CE, which may naturally explain the observed planetary masses. In addition, hybrid scenarios where the planets form before the CE and evolve due to the accretion of the ejected gas appear as a realistic possibility.

  1. Summary of Historical Production for Nevada Binary Facilities

    SciTech Connect (OSTI)

    Mines, Greg; Hanson, Hillary

    2001-09-01T23:59:59.000Z

    The analysis described was initiated to validate inputs used in the US Department of Energy’s (DOE) economic modeling tool GETEM (Geothermal Electricity Technology Evaluation Model) by using publically available data to identify production trends at operating geothermal binary facilities in the state of Nevada. Data required for this analysis was obtained from the Nevada Bureau of Mines and Geology (NBMG), whom received the original operator reports from the Nevada Division of Minerals (NDOM). The data from the NBMG was inputted into Excel files that have been uploaded to the DOE’s National Geothermal Data System (NGDS). Once data was available in an Excel format, production trends for individual wells and facilities could be established for the periods data was available (thru 2009). Additionally, this analysis identified relationships existing between production (temperature and flow rates), power production and plant conversion efficiencies. The data trends showed that temperature declines have a significant impact on power production, and that in some instances operators increased production flow rate to offset power declines. The production trends with time that were identified are being used to update GETEM’s default inputs.

  2. Monolithic Active Pixel Matrix with Binary Counters (MAMBO) ASIC

    SciTech Connect (OSTI)

    Khalid, Farah F.; Deptuch, Grzegorz; Shenai, Alpana; Yarema, Raymond J.; /Fermilab

    2010-11-01T23:59:59.000Z

    Monolithic Active Matrix with Binary Counters (MAMBO) is a counting ASIC designed for detecting and measuring low energy X-rays from 6-12 keV. Each pixel contains analogue functionality implemented with a charge preamplifier, CR-RC{sup 2} shaper and a baseline restorer. It also contains a window comparator which can be trimmed by 4 bit DACs to remove systematic offsets. The hits are registered by a 12 bit ripple counter which is reconfigured as a shift register to serially output the data from the entire ASIC. Each pixel can be tested individually. Two diverse approaches have been used to prevent coupling between the detector and electronics in MAMBO III and MAMBO IV. MAMBO III is a 3D ASIC, the bottom ASIC consists of diodes which are connected to the top ASIC using {mu}-bump bonds. The detector is decoupled from the electronics by physically separating them on two tiers and using several metal layers as a shield. MAMBO IV is a monolithic structure which uses a nested well approach to isolate the detector from the electronics. The ASICs are being fabricated using the SOI 0.2 {micro}m OKI process, MAMBO III is 3D bonded at T-Micro and MAMBO IV nested well structure was developed in collaboration between OKI and Fermilab.

  3. Summary of Historical Production for Nevada Binary Facilities

    SciTech Connect (OSTI)

    Mines, Greg; Hanson, Hillary

    2014-09-01T23:59:59.000Z

    The analysis described was initiated to validate inputs used in the US Department of Energy’s (DOE) economic modeling tool GETEM (Geothermal Electricity Technology Evaluation Model) by using publically available data to identify production trends at operating geothermal binary facilities in the state of Nevada. Data required for this analysis was obtained from the Nevada Bureau of Mines and Geology (NBMG), whom received the original operator reports from the Nevada Division of Minerals (NDOM). The data from the NBMG was inputted into Excel files that have been uploaded to the DOE’s National Geothermal Data System (NGDS). Once data was available in an Excel format, production trends for individual wells and facilities could be established for the periods data was available (thru 2009). Additionally, this analysis identified relationships existing between production (temperature and flow rates), power production and plant conversion efficiencies. The data trends showed that temperature declines have a significant impact on power production, and that in some instances operators increased production flow rate to offset power declines. The production trends with time that were identified are being used to update GETEM’s default inputs.

  4. Magnetic energy production by turbulence in binary neutron star mergers

    E-Print Network [OSTI]

    Zrake, Jonathan

    2013-01-01T23:59:59.000Z

    The simultaneous detection of electromagnetic and gravitational wave emission from merging neutron star binaries would aid greatly in their discovery and interpretation. By studying turbulent amplification of magnetic fields in local high-resolution simulations of neutron star merger conditions, we demonstrate that magnetar-level (~10^16) G fields are present throughout the merger duration. We find that the small-scale turbulent dynamo converts 60% of the randomized kinetic energy into magnetic fields on a merger time scale. Since turbulent magnetic energy dissipates through reconnection events which accelerate relativistic electrons, turbulence may facilitate the conversion of orbital kinetic energy into radiation. If 10^-4 of the ~ 10^53 erg of orbital kinetic available gets processed through reconnection, and creates radiation in the 15-150 keV band, then the fluence at 200 Mpc would be 10^-7 erg/cm^2, potentially rendering most merging neutron stars in the advanced LIGO and Virgo detection volumes detecta...

  5. Preliminary study of pseudorandom binary sequence pulsing of ORELA

    SciTech Connect (OSTI)

    Larson, N. M.; Olsen, D. K.

    1980-03-01T23:59:59.000Z

    It has been suggested that pseudorandom binary sequence (PRBS) pulsing might enhance the performance of the Oak Ridge Electron Linear Accelerator (ORELA) for neutron-induced, time-of-flight (TOF) cross-section measurements. In this technical memorandum, equations are developed for expected count rates, statistical variances, and backgrounds for a pulsing scheme in which a PRBS is superimposed on the periodic equalintensity ORELA bursts. Introduction of the PRBS modification permits neutrons of different energies originating from different bursts to reach the detector simultaneously, and the signal corresponding to a unique flight time to be extracted mathematically. Relative advantages and disadvantages of measurements from conventional and PRBS pulsing modes are discussed in terms of counting statistics and backgrounds. Computer models of TOF spectra are generated for both pulsing modes, using as examples a 20-meter /sup 233/U fission-chamber measurement and a 155-meter /sup 238/U sample-in transmission measurement. Detailed comparisons of PRBS vs conventional results are presented. This study indicates that although PRBS pulsing could enhance ORELA performance for selected measurements, for general ORELA operation the disadvantages from PRBS pulsing probably outweigh the advantages.

  6. Comprehensive nucleosynthesis analysis for ejecta of compact binary mergers

    E-Print Network [OSTI]

    Just, Oliver; Pulpillo, Ricard Ardevol; Goriely, Stephane; Janka, H -Thomas

    2015-01-01T23:59:59.000Z

    We present a comprehensive study of r-process element nucleosynthesis in the ejecta of compact binary mergers (CBMs) and their relic black-hole (BH)-torus systems. The evolution of the BH-accretion tori is simulated for seconds with a Newtonian hydrodynamics code including viscosity effects, pseudo-Newtonian gravity for rotating BHs, and an energy-dependent two-moment closure scheme for the transport of electron neutrinos and antineutrinos. The investigated cases are guided by relativistic double neutron star (NS-NS) and NS-BH merger models, producing ~3-6 Msun BHs with rotation parameters of A~0.8 and tori of 0.03-0.3 Msun. Our nucleosynthesis analysis includes the dynamical (prompt) ejecta expelled during the CBM phase and the neutrino and viscously driven outflows of the relic BH-torus systems. While typically ~20-25% of the initial accretion-torus mass are lost by viscously driven outflows, neutrino-powered winds contribute at most another ~1%, but neutrino heating enhances the viscous ejecta significantl...

  7. COSMOLOGICAL FAST RADIO BURSTS FROM BINARY WHITE DWARF MERGERS

    SciTech Connect (OSTI)

    Kashiyama, Kazumi; Mészáros, Peter [Department of Astronomy and Astrophysics, Department of Physics, Center for Particle and Gravitational Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States)] [Department of Astronomy and Astrophysics, Department of Physics, Center for Particle and Gravitational Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States); Ioka, Kunihito, E-mail: kzk15@psu.edu, E-mail: nnp@psu.edu, E-mail: kunihito.ioka@kek.jp [Theory Center, Institute of Particle and Nuclear Studies, KEK, Department of Particle and Nuclear Physics, the Graduate University for Advanced Studies (Sokendai), Tsukuba 305-0801 (Japan)] [Theory Center, Institute of Particle and Nuclear Studies, KEK, Department of Particle and Nuclear Physics, the Graduate University for Advanced Studies (Sokendai), Tsukuba 305-0801 (Japan)

    2013-10-20T23:59:59.000Z

    Recently, Thornton et al. reported the detection of four fast radio bursts (FRBs). The dispersion measures indicate that the sources of these FRBs are at cosmological distance. Given the large full sky event rate ?10{sup 4} sky{sup –1} day{sup –1}, the FRBs are a promising target for multi-messenger astronomy. Here we propose double degenerate, binary white-dwarf (WD) mergers as the source of FRBs, which are produced by coherent emission from the polar region of a rapidly rotating, magnetized massive WD formed after the merger. The basic characteristics of the FRBs, such as the energetics, emission duration and event rate, can be consistently explained in this scenario. As a result, we predict that some FRBs can accompany type Ia supernovae (SNe Ia) or X-ray debris disks. Simultaneous detection could test our scenario and probe the progenitors of SNe Ia, and moreover would provide a novel constraint on the cosmological parameters. We strongly encourage future SN and X-ray surveys that follow up FRBs.

  8. Faint Thermonuclear Supernovae from AM Canum Venaticorum Binaries

    E-Print Network [OSTI]

    Lars Bildsten; Ken J. Shen; Nevin N. Weinberg; Gijs Nelemans

    2007-05-06T23:59:59.000Z

    Helium that accretes onto a Carbon/Oxygen white dwarf in the double white dwarf AM Canum Venaticorum (AM CVn) binaries undergoes unstable thermonuclear flashes when the orbital period is in the 3.5-25 minute range. At the shortest orbital periods (and highest accretion rates, Mdot > 10^-7 Msol/yr), the flashes are weak and likely lead to the Helium equivalent of classical nova outbursts. However, as the orbit widens and Mdot drops, the mass required for the unstable ignition increases, leading to progressively more violent flashes up to a final flash with Helium shell mass ~ 0.02-0.1 Msol. The high pressures of these last flashes allow the burning to produce the radioactive elements 48Cr, 52Fe, and 56Ni that power a faint (M_V in the range of -15 to -18) and rapidly rising (few days) thermonuclear supernova. Current galactic AM CVn space densities imply one such explosion every 5,000-15,000 years in 10^11 Msol of old stars (~ 2-6% of the Type Ia rate in E/SO galaxies). These ".Ia" supernovae (one-tenth as bright for one-tenth the time as a Type Ia supernovae) are excellent targets for deep (e.g. V=24) searches with nightly cadences, potentially yielding an all-sky rate of 1,000 per year.

  9. Magnetically-induced outflows from binary neutron star merger remnants

    E-Print Network [OSTI]

    Daniel M. Siegel; Riccardo Ciolfi

    2015-05-06T23:59:59.000Z

    Recent observations by the Swift satellite have revealed long-lasting ($\\sim 10^2-10^5\\,\\mathrm{s}$), "plateau-like" X-ray afterglows in the vast majority of short gamma-ray bursts events. This has put forward the idea of a long-lived millisecond magnetar central engine being generated in a binary neutron star (BNS) merger and being responsible for the sustained energy injection over these timescales ("magnetar model"). We elaborate here on recent simulations that investigate the early evolution of such a merger remnant in general-relativistic magnetohydrodynamics. These simulations reveal very different conditions than those usually assumed for dipole spin-down emission in the magnetar model. In particular, the surrounding of the newly formed NS is polluted by baryons due to a dense, highly magnetized and isotropic wind from the stellar surface that is induced by magnetic field amplification in the interior of the star. The timescales and luminosities of this wind are compatible with early X-ray afterglows, such as the "extended emission". These isotropic winds are a generic feature of BNS merger remnants and thus represent an attractive alternative to current models of early X-ray afterglows. Further implications to BNS mergers and short gamma-ray bursts are discussed.

  10. On q-deformed Stirling numbers

    E-Print Network [OSTI]

    Yilmaz Simsek

    2007-11-03T23:59:59.000Z

    The purpose of this article is to introduce q-deformed Stirling numbers of the first and second kinds. Relations between these numbers, Riemann zeta function and q-Bernoulli numbers of higher order are given. Some relations related to the classical Stirling numbers and Bernoulli numbers of higher order are found. By using derivative operator to the generating function of the q-deformed Stirling numbers of the second kinds, a new function is defined which interpolates the q-deformed Stirling numbers of the second kinds at negative integers. The recurrence relations of the Stirling numbers of the first and second kind are given. In addition, relation between q-deformed Stirling numbers and q-Bell numbers is obtained.

  11. Verification Challenges at Low Numbers

    SciTech Connect (OSTI)

    Benz, Jacob M.; Booker, Paul M.; McDonald, Benjamin S.

    2013-06-01T23:59:59.000Z

    Many papers have dealt with the political difficulties and ramifications of deep nuclear arms reductions, and the issues of “Going to Zero”. Political issues include extended deterrence, conventional weapons, ballistic missile defense, and regional and geo-political security issues. At each step on the road to low numbers, the verification required to ensure compliance of all parties will increase significantly. Looking post New START, the next step will likely include warhead limits in the neighborhood of 1000 . Further reductions will include stepping stones at1000 warheads, 100’s of warheads, and then 10’s of warheads before final elimination could be considered of the last few remaining warheads and weapons. This paper will focus on these three threshold reduction levels, 1000, 100’s, 10’s. For each, the issues and challenges will be discussed, potential solutions will be identified, and the verification technologies and chain of custody measures that address these solutions will be surveyed. It is important to note that many of the issues that need to be addressed have no current solution. In these cases, the paper will explore new or novel technologies that could be applied. These technologies will draw from the research and development that is ongoing throughout the national laboratory complex, and will look at technologies utilized in other areas of industry for their application to arms control verification.

  12. Grant Title: INNOVATIVE TECHNOLOGY EXPERIENCES FOR STUDENTS AND TEACHERS (ITEST) Funding Opportunity Number: NSF 12-597. CFDA Number(s): 47.076.

    E-Print Network [OSTI]

    Farritor, Shane

    Opportunity Number: NSF 12-597. CFDA Number(s): 47.076. Agency/Department: National Science Foundation

  13. Prime number generation and factor elimination

    E-Print Network [OSTI]

    Vineet Kumar

    2014-10-06T23:59:59.000Z

    We have presented a multivariate polynomial function termed as factor elimination function,by which, we can generate prime numbers. This function's mapping behavior can explain the irregularities in the occurrence of prime numbers on the number line. Generally the different categories of prime numbers found till date, satisfy the form of this function. We present some absolute and probabilistic conditions for the primality of the number generated by this method. This function is capable of leading to highly efficient algorithms for generating prime numbers.

  14. X-RAY BINARY EVOLUTION ACROSS COSMIC TIME

    SciTech Connect (OSTI)

    Fragos, T.; Zezas, A. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)] [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Lehmer, B.; Tzanavaris, P. [Department of Physics and Astronomy, The Johns Hopkins University, Homewood Campus, Baltimore, MD 21218 (United States)] [Department of Physics and Astronomy, The Johns Hopkins University, Homewood Campus, Baltimore, MD 21218 (United States); Tremmel, M. [Department of Astronomy, University of Washington, Box 351580, U.W., Seattle, WA 98195-1580 (United States)] [Department of Astronomy, University of Washington, Box 351580, U.W., Seattle, WA 98195-1580 (United States); Basu-Zych, A.; Hornschemeier, A.; Jenkins, L.; Ptak, A. [NASA Goddard Space Flight Centre, Code 662, Greenbelt, MD 20771 (United States)] [NASA Goddard Space Flight Centre, Code 662, Greenbelt, MD 20771 (United States); Belczynski, K. [Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, 00-478 Warsaw (Poland)] [Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, 00-478 Warsaw (Poland); Kalogera, V., E-mail: tfragos@cfa.harvard.edu [Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208 (United States)

    2013-02-10T23:59:59.000Z

    High-redshift galaxies permit the study of the formation and evolution of X-ray binary (XRB) populations on cosmological timescales, probing a wide range of metallicities and star formation rates (SFRs). In this paper, we present results from a large-scale population synthesis study that models the XRB populations from the first galaxies of the universe until today. We use as input to our modeling the Millennium II cosmological simulation and the updated semi-analytic galaxy catalog by Guo et al. to self-consistently account for the star formation history and metallicity evolution of the universe. Our modeling, which is constrained by the observed X-ray properties of local galaxies, gives predictions about the global scaling of emission from XRB populations with properties such as SFR and stellar mass, and the evolution of these relations with redshift. Our simulations show that the X-ray luminosity density (X-ray luminosity per unit volume) from XRBs in our universe today is dominated by low-mass XRBs, and it is only at z {approx}> 2.5 that high-mass XRBs become dominant. We also find that there is a delay of {approx}1.1 Gyr between the peak of X-ray emissivity from low-mass XRBs (at z {approx} 2.1) and the peak of SFR density (at z {approx} 3.1). The peak of the X-ray luminosity from high-mass XRBs (at z {approx} 3.9) happens {approx}0.8 Gyr before the peak of the SFR density, which is due to the metallicity evolution of the universe.

  15. Binary electrokinetic separation of target DNA from background DNA primers.

    SciTech Connect (OSTI)

    James, Conrad D.; Derzon, Mark Steven

    2005-10-01T23:59:59.000Z

    This report contains the summary of LDRD project 91312, titled ''Binary Electrokinetic Separation of Target DNA from Background DNA Primers''. This work is the first product of a collaboration with Columbia University and the Northeast BioDefense Center of Excellence. In conjunction with Ian Lipkin's lab, we are developing a technique to reduce false positive events, due to the detection of unhybridized reporter molecules, in a sensitive and multiplexed detection scheme for nucleic acids developed by the Lipkin lab. This is the most significant problem in the operation of their capability. As they are developing the tools for rapidly detecting the entire panel of hemorrhagic fevers this technology will immediately serve an important national need. The goal of this work was to attempt to separate nucleic acid from a preprocessed sample. We demonstrated the preconcentration of kilobase-pair length double-stranded DNA targets, and observed little preconcentration of 60 base-pair length single-stranded DNA probes. These objectives were accomplished in microdevice formats that are compatible with larger detection systems for sample pre-processing. Combined with Columbia's expertise, this technology would enable a unique, fast, and potentially compact method for detecting/identifying genetically-modified organisms and multiplexed rapid nucleic acid identification. Another competing approach is the DARPA funded IRIS Pharmaceutical TIGER platform which requires many hours for operation, and an 800k$ piece of equipment that fills a room. The Columbia/SNL system could provide a result in 30 minutes, at the cost of a few thousand dollars for the platform, and would be the size of a shoebox or smaller.

  16. Do X-ray Binary Spectral State Transition Luminosities Vary?

    E-Print Network [OSTI]

    Thomas J. Maccarone

    2003-08-02T23:59:59.000Z

    We tabulate the luminosities of the soft-to-hard state transitions of all X-ray binaries for which there exist good X-ray flux measurements at the time of the transition, good distance estimates, and good mass estimates for the compact star. We show that the state transition luminosities are at about 1-4% of the Eddington rate, markedly smaller than those typically quoted in the literature, with a mean value of 2%. Only the black hole candidate GRO J~1655-40 and the neutron star systems Aql X-1 and 4U 1728-34 have measured state transition luminosities inconsistent with this value at the 1$\\sigma$ level. GRO J~1655-40, in particular, shows a state transition luminosity below the mean value for the other sources at the $4\\sigma$ level. This result, combined with the known inner disk inclination angle (the disk is nearly parallel to the line of sight) from GRO J~1655-40's relativistic jets suggest that the hard X-ray emitting region in GRO J~1655-40 can have a velocity of no more than about $\\beta=0.68$, with a most likely value of about $\\beta=0.52$, and a minimum speed of $\\beta=0.45$, assuming that the variations in state transition luminosities are solely due to relativistic beaming effects. The variance in the state transition luminosities suggests an emission region with a velocity of $\\sim0.2c$. The results are discussed in terms of different emission models for the low/hard state. We also discuss the implications for measuring the dimensionless viscosity parameter $\\alpha$. We also find that if its state transitions occur at typical luminosities, then GX 339-4 is likely to be at a distance of at least 7.6 kpc, much further than typically quoted estimates.

  17. Turing's normal numbers: towards randomness Veronica Becher

    E-Print Network [OSTI]

    presumably in 1938 Alan Turing gave an algorithm that produces real numbers normal to every integer base- putable normal numbers, and this result should be attributed to Alan Turing. His manuscript entitled "A

  18. WIYN open cluster study. LX. Spectroscopic binary orbits in NGC 6819

    SciTech Connect (OSTI)

    Milliman, Katelyn E.; Mathieu, Robert D.; Gosnell, Natalie M. [Department of Astronomy, University of Wisconsin-Madison, 475 North Charter Street Madison, WI 53706 (United States); Geller, Aaron M. [Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, 2145 Sheridan Road, Evanston, IL 60208 (United States); Meibom, Søren [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Platais, Imants, E-mail: milliman@astro.wisc.edu [Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218 (United States)

    2014-08-01T23:59:59.000Z

    We present the current state of the WOCS radial-velocity (RV) survey for the rich open cluster NGC 6819 (2.5 Gyr) including 93 spectroscopic binary orbits with periods ranging from 1.5 to 8000 days. These results are the product of our ongoing RV survey of NGC 6819 using the Hydra Multi-Object Spectrograph on the WIYN 3.5 m telescope. We also include a detailed analysis of multiple prior sets of optical photometry for NGC 6819. Within a 1° field of view, our stellar sample includes the giant branch, the red clump, and blue straggler candidates, and extends to almost 2 mag below the main sequence (MS) turnoff. For each star observed in our survey we present all RV measurements, the average RV, and velocity variability information. Additionally, we discuss notable binaries from our sample, including eclipsing binaries (WOCS 23009, WOCS 24009, and WOCS 40007), stars noted in Kepler asteroseismology studies (WOCS 4008, WOCS 7009, and WOCS 8007), and potential descendants of past blue stragglers (WOCS 1006 and WOCS 6002). We find the incompleteness-corrected binary fraction for all MS binaries with periods less than 10{sup 4} days to be 22% ± 3% and a tidal circularization period of 6.2{sub ?1.1}{sup +1.1} days for NGC 6819.

  19. Recoils from unequal-mass, precessing black-hole binaries: The Intermediate Mass Ratio Regime

    E-Print Network [OSTI]

    Zlochower, Yosef

    2015-01-01T23:59:59.000Z

    We revisit the modeling of the properties of the black-hole remnant resulting the merger of a black-hole binary as a function of the parameters of the binary. We provide a set of empirical formulas for the final mass, spin and recoil velocity of the final black hole as a function of the mass ratio and individual spins of the progenitor. In order to determine the fitting coefficients for these formulas, we perform a set of 126 new numerical evolutions of precessing, unequal-mass black-hole binaries, and fit to the resulting remnant mass, spin, and recoil. In order to reduce the complexity of the analysis, we chose configurations that have one of the black holes spinning, with dimensionless spin alpha=0.8, at different angles with respect to the orbital angular momentum, and the other non-spinning. In addition to evolving families of binaries with different spin-inclination angles, we also evolved binaries with mass ratios as small as q=1/6. We use the resulting empirical formulas to predict the probabilities o...

  20. EXPECTED LARGE SYNOPTIC SURVEY TELESCOPE (LSST) YIELD OF ECLIPSING BINARY STARS

    SciTech Connect (OSTI)

    Prsa, Andrej [Department of Astronomy and Astrophysics, Villanova University, 800 East Lancaster Avenue, Villanova, PA 19085 (United States); Pepper, Joshua; Stassun, Keivan G., E-mail: andrej.prsa@villanova.edu [Physics and Astronomy Department, Vanderbilt University, 2201 West End Avenue, Nashville, TN 37235 (United States)

    2011-08-15T23:59:59.000Z

    In this paper, we estimate the Large Synoptic Survey Telescope (LSST) yield of eclipsing binary stars, which will survey {approx}20,000 deg{sup 2} of the southern sky during a period of 10 years in six photometric passbands to r {approx} 24.5. We generate a set of 10,000 eclipsing binary light curves sampled to the LSST time cadence across the whole sky, with added noise as a function of apparent magnitude. This set is passed to the analysis-of-variance period finder to assess the recoverability rate for the periods, and the successfully phased light curves are passed to the artificial-intelligence-based pipeline ebai to assess the recoverability rate in terms of the eclipsing binaries' physical and geometric parameters. We find that, out of {approx}24 million eclipsing binaries observed by LSST with a signal-to-noise ratio >10 in mission lifetime, {approx}28% or 6.7 million can be fully characterized by the pipeline. Of those, {approx}25% or 1.7 million will be double-lined binaries, a true treasure trove for stellar astrophysics.

  1. An alternative parameterisation for binary-lens caustic-crossing events

    E-Print Network [OSTI]

    A. Cassan

    2008-10-15T23:59:59.000Z

    Microlensing events are being discovered and alerted by the two survey teams OGLE and MOA at an increasing rate. Around ten percent of these events involve binary lenses. Such events potentially contain much information on the physical properties of the observed binary systems, which can then be used for e.g. statistical studies on binary objects in the Galactic disk or bulge. However, such events are usually not straightforward to study, because the model equations are strongly non-linear and there are many local minima that can fool the search for the best solution if the parameter space is not inspected with great care. In this work an alternative parameterisation for the binary lens fitting problem is proposed, in which the parameters involved are defined to represent as closely as possible the caustic-crossing features observed in most binary lens light curves. Furthermore, we work out an extension of the method in order to make use of the straight line fold caustic approximation, when the latter applies for both the caustic entry and exit. We introduce an alternative parameterisation in order to confine the exploration of the parameter space to regions where the models only involve caustic crossing at the dates seen in the light curve. We find that the proposed parameterisation provides more robustness to the light curve fitting process, in particular in avoiding a code to get stuck in false minima.

  2. Spin alignment and differential accretion in merging black-hole binaries

    E-Print Network [OSTI]

    Gerosa, Davide; Lodato, Giuseppe; Rosotti, Giovanni

    2015-01-01T23:59:59.000Z

    Interactions between a supermassive black-hole binary and the surrounding accretion disc can both assist the binary inspiral and align the black-hole spins to the disc angular momentum. While binary migration is due to angular-momentum transfer within the circumbinary disc, the spin-alignment process is driven by the mass accreting onto each black hole. Mass transfer between different disc components thus couples the inspiral and the alignment process together. Mass is expected to leak through the cavity cleared by the binary, and preferentially accretes onto the lighter (secondary) black-hole which orbits closer to the disc edge. Low accretion rate onto the heavier (primary) black hole slows the alignment process down. We revisit the problem and develop a semi-analytical model to describe the coupling between gas-driven inspiral and spin alignment, finding that binaries with mass ratio q<~0.2 approach the gravitational-wave driven inspiral in differential misalignment: light secondaries prevent primaries ...

  3. High speed optical quantum random number generation

    E-Print Network [OSTI]

    Weinfurter, Harald

    .3351 (2009). 6. I. Reidler, Y. Aviad, M. Rosenbluh, and I. Kanter, "Ultrahigh-speed random number generation

  4. Clar number of catacondensed benzenoid hydrocarbons

    E-Print Network [OSTI]

    Klavzar, Sandi

    Clar number of catacondensed benzenoid hydrocarbons Sandi KlavŸzar a,# , Petra Ÿ Zigert a , Ivan hydrocarbon: CL is equal to the minimum number of straight lines required to intersect all hexagons theory; Clar formula; Clar number; Resonance graph; Benzenoid hydrocarbons 1. Introduction Within

  5. The Gravitational Wave Background From Coalescing Compact Binaries: A New Method

    E-Print Network [OSTI]

    Evangelista, E F D

    2015-01-01T23:59:59.000Z

    Gravitational waves are perturbations in the spacetime that propagate at the speed of light. The study of such phenomenon is interesting because many cosmological processes and astrophysical objects, such as binary systems, are potential sources of gravitational radiation and can have their emissions detected in the near future by the next generation of interferometric detectors. Concerning the astrophysical objects, an interesting case is when there are several sources emitting in such a way that there is a superposition of signals, resulting in a smooth spectrum which spans a wide range of frequencies, the so-called stochastic background. In this paper, we are concerned with the stochastic backgrounds generated by compact binaries (i.e. binary systems formed by neutron stars and black holes) in the coalescing phase. In particular, we obtain such backgrounds by employing a new method developed in our previous studies.

  6. Optimality of binary power-control in a single cell via majorization

    E-Print Network [OSTI]

    Inaltekin, Hazer

    2011-01-01T23:59:59.000Z

    This paper considers the optimum single cell power-control maximizing the aggregate (uplink) communication rate of the cell when there are peak power constraints at mobile users, and a low-complexity data decoder (without successive decoding) at the base station. It is shown, via the theory of majorization, that the optimum power allocation is binary, which means links are either "on" or "off". By exploiting further structure of the optimum binary power allocation, a simple polynomial-time algorithm for finding the optimum transmission power allocation is proposed, together with a reduced complexity near-optimal heuristic algorithm. Sufficient conditions under which channel-state aware time-division-multiple-access (TDMA) maximizes the aggregate communication rate are established. Finally, a numerical study is performed to compare and contrast the performance achieved by the optimum binary power-control policy with other sub-optimum policies and the throughput capacity achievable via successive decoding. It i...

  7. Wide Binary Effects on Asymmetries in Asymptotic Giant Branch Circumstellar Envelopes

    E-Print Network [OSTI]

    Kim, Hyosun

    2012-01-01T23:59:59.000Z

    Observations of increasingly higher spatial resolution reveal the existence of asymmetries in the circumstellar envelopes of a small fraction of asymptotic giant branch (AGB) stars. Although there is no general consensus for their origin, a binary companion star may be responsible. Within this framework, we investigate the gravitational effects associated with a sufficiently wide binary system, where Roche lobe overflow is unimportant, on the outflowing envelopes of AGB stars using three dimensional hydrodynamic simulations. The effects due to individual binary components are separately studied, enabling investigation of the stellar and circumstellar characteristics in detail. The reflex motion of the AGB star alters the wind velocity distribution, thereby, determining the overall shape of the outflowing envelope. On the other hand, the interaction of the companion with the envelope produces a gravitational wake, which exhibits a vertically thinner shape. The two patterns overlap and form clumpy structures. T...

  8. Effect of Ambient Design Temperature on Air-Cooled Binary Plant Output

    SciTech Connect (OSTI)

    Dan Wendt; Greg Mines

    2011-10-01T23:59:59.000Z

    Air-cooled binary plants are designed to provide a specified level of power production at a particular air temperature. Nominally this air temperature is the annual mean or average air temperature for the plant location. This study investigates the effect that changing the design air temperature has on power generation for an air-cooled binary plant producing power from a resource with a declining production fluid temperature and fluctuating ambient temperatures. This analysis was performed for plants operating both with and without a geothermal fluid outlet temperature limit. Aspen Plus process simulation software was used to develop optimal air-cooled binary plant designs for specific ambient temperatures as well as to rate the performance of the plant designs at off-design operating conditions. Results include calculation of annual and plant lifetime power generation as well as evaluation of plant operating characteristics, such as improved power generation capabilities during summer months when electric power prices are at peak levels.

  9. The Runaway Binary LP 400-22 is Leaving the Galaxy

    E-Print Network [OSTI]

    Kilic, Mukremin; Brown, Warren R; Harris, Hugh C; Dahn, Conard C; Agueros, M A; Heinke, Craig O; Kenyon, S J; Panei, J A; Camilo, Fernando

    2013-01-01T23:59:59.000Z

    We present optical spectroscopy, astrometry, radio, and X-ray observations of the runaway binary LP 400-22. We refine the orbital parameters of the system based on our new radial velocity observations. Our parallax data indicate that LP 400-22 is significantly more distant (3 sigma lower limit of 840 pc) than initially predicted. LP 400-22 has a tangential velocity in excess of 830 km/s; it is unbound to the Galaxy. Our radio and X-ray observations fail to detect a recycled millisecond pulsar companion, indicating that LP 400-22 is a double white dwarf system. This essentially rules out a supernova runaway ejection mechanism. Based on its orbit, a Galactic center origin is also unlikely. However, its orbit intersects the locations of several globular clusters; dynamical interactions between LP 400-22 and other binary stars or a central black hole in a dense cluster could explain the origin of this unusual binary.

  10. Warping and tearing of misaligned circumbinary disks around eccentric SMBH binaries

    E-Print Network [OSTI]

    Hayasaki, Kimitake; Okazaki, Atsuo T; Jung, Taehyun; Zhao, Guangyao; Naito, Tsuguya

    2015-01-01T23:59:59.000Z

    We study the warping and tearing of a geometrically thin, non-self-gravitating disk surrounding binary supermassive black holes on an eccentric orbit. The circumbinary disk is significantly misaligned with the binary orbital plane, and is subject to the time-dependent tidal torques. In principle, such a disk is warped and precesses, and is torn into mutually misaligned rings in the region, where the tidal precession torques are stronger than the local viscous torques. We derive the tidal-warp and tearing radii of the misaligned circumbinary disks around eccentric SMBH binaries. We find that in disks with the viscosity parameter, alpha, larger than a critical value depending on the disk aspect ratio, the disk warping appears outside the tearing radius. This condition is expressed as alpha > sqrt{H/3r} for H/r ~material is likely to rapi...

  11. Secular variability, geodetic precession and moment of inertia of binary pulsars

    E-Print Network [OSTI]

    B. P. Gong

    2003-06-04T23:59:59.000Z

    More and more binary pulsars show significant secular variations, in which the measured projected semi-major axis, $\\dot{x}^{obs}$, and the first derivative of orbital period, $\\dot{P}_{b}^{obs}$, are several order of magnitude larger than the prediction of general relativity (GR). This paper shows that the geodetic precession induced orbital effects can explain both $\\dot{x}$ and $\\dot{P}_{b}$ measured in binary pulsars. Moreover, by this model we can automatically estimate the magnitude of the spin angular momenta of the pulsar and its companion star, and therefore the moment of inertia ($10^{44}$g cm$^2$ to $10^{45}$g cm$^2$) of pulsar of binary pulsar systems, which agrees well with theoretical predictions. In other words, the contamination (residual represented by $\\dot{x}$ and $\\dot{P}_{b}$) in pulsar timing measurements might be caused by geodetic precession, an interesting gravitational effect we have been seeking for.

  12. Tip sheet: Expanded Library of Congress Call Number Classification system Call Number Subject Matter

    E-Print Network [OSTI]

    Kambhampati, Patanjali

    Tip sheet: Expanded Library of Congress Call Number Classification system Call Number Subject R: Medicine T: Technology U: Military Science Z: Bibliography. Library Science. Information

  13. Accurate Computer Simulation of Phase Equilibrium for Complex Fluid Mixtures. Application to Binaries Involving Isobutene, Methanol, Methyl tert-Butyl Ether, and

    E-Print Network [OSTI]

    Lisal, Martin

    to Binaries Involving Isobutene, Methanol, Methyl tert-Butyl Ether, and n-Butane Martin Li´sal,*,, William R + methyl tert-butyl ether (MTBE) and the binaries formed by methanol with isobutene, MTBE, and n

  14. A three-dimensional model for particle dissolution in binary alloys F.J. Vermolen a,*, E. Javierre a

    E-Print Network [OSTI]

    Vuik, Kees

    A three-dimensional model for particle dissolution in binary alloys F.J. Vermolen a,*, E. Javierre, Department of Aerospace Engineering, Kluyverweg 1, 2629 HS Delft, The Netherlands Received 13 September 2006; accepted 20 September 2006 Abstract A three-dimensional model for particle dissolution in binary alloys

  15. A STABILIZED VOLUME-AVERAGING FINITE ELEMENT METHOD FOR FLOW IN POROUS MEDIA AND BINARY ALLOY SOLIDIFICATION SYSTEMS

    E-Print Network [OSTI]

    Zabaras, Nicholas J.

    A STABILIZED VOLUME-AVERAGING FINITE ELEMENT METHOD FOR FLOW IN POROUS MEDIA AND BINARY ALLOY of Mechanical and Aerospace Engineering 188 Frank H. T. Rhodes Hall Cornell University Ithaca, NY 14853 algorithm is presented for the analysis of flow in porous media and in the solidification of binary alloys

  16. The Ising model and critical behavior of transport in binary composite N. B. Murphy and K. M. Golden

    E-Print Network [OSTI]

    Golden, Kenneth M.

    nanotube composites,37 and sea ice.26,27 A key feature of these materials is the critical dependenceThe Ising model and critical behavior of transport in binary composite media N. B. Murphy and K. M) The Ising model and critical behavior of transport in binary composite media N. B. Murphy and K. M. Golden

  17. ISIT 2002, Lausanne, Switzerland, June 30 July 5, 2002 Matched Information Rate Codes for Binary ISI channels1

    E-Print Network [OSTI]

    Kavcic, Aleksandar

    ISI channels1 Xiao Ma, Nedeljko Varnica and Aleksandar Kavci´c DEAS/Harvard University, Cambridge, MA- proach the channel capacities for binary intersymbol interfer- ence (ISI) channels. The proposed codes-check (LDPC) codes. The whole system is it- eratively decodable. I. SUMMARY Binary ISI channel models

  18. ISIT 2002, Lausanne, Switzerland, June 30 --July 5, 2002 Matched Information Rate Codes for Binary ISI channels 1

    E-Print Network [OSTI]

    Kavcic, Aleksandar

    ISI channels 1 Xiao Ma, Nedeljko Varnica and Aleksandar KavŸciâ??c DEAS/Harvard University, Cambridge to ap­ proach the channel capacities for binary intersymbol interfer­ ence (ISI) channels. The proposed­density parity­check (LDPC) codes. The whole system is it­ eratively decodable. I. SUMMARY Binary ISI channel

  19. The first light-curve analysis of eclipsing binaries observed by the INTEGRAL/OMC

    E-Print Network [OSTI]

    P. Zasche

    2008-04-24T23:59:59.000Z

    Three Algol-type binaries in Cygnus constellation were selected for an analysis from a huge database of observations made by the INTEGRAL/OMC camera. These data were processed and analyzed, resulting in a first light-curve study of these neglected eclipsing binaries. The temperatures of the primary components range from 9500 K to 10500 K and the inclinations are circa 73deg (for PV Cyg and V1011 Cyg), while almost 90deg for V822 Cyg. All of them seem to be main-sequence stars, well within their critical Roche lobes. Nevertheless, further detailed analyses are still needed.

  20. Binary and ternary gas mixtures for use in glow discharge closing switches

    DOE Patents [OSTI]

    Hunter, S.R.; Christophorou, L.G.

    1988-04-27T23:59:59.000Z

    Highly efficient binary and ternary gas mixtures for use in diffuse glow discharge closing switches are disclosed. The binary mixtures are combinations of helium or neon and selected perfluorides. The ternary mixtures are combinations of helium, neon, or argon, a selected perfluoride, and a small amount of gas that exhibits enhanced ionization characteristics. These mixtures are shown to be the optimum choices for use in diffuse glow discharge closing switches by virtue if the combines physio-electric properties of the mixture components. 9 figs.

  1. THE HOT R CORONAE BOREALIS STAR DY CENTAURI IS A BINARY

    SciTech Connect (OSTI)

    Kameswara Rao, N. [543, 17th Main, IV Sector, HSR Layout, Bangalore 560102 (India); Lambert, David L.; McArthur, Barbara [W. J. McDonald Observatory, University of Texas, Austin, TX 78712-1083 (United States); Garcia-Hernandez, D. A. [Instituto de Astrofisica de Canarias, C/Via Lactea s/n, E-38205 La Laguna (Spain); Simon Jeffery, C. [Armagh Observatory, College Hill, Armagh BT61 9DG (United Kingdom); Woolf, Vincent M., E-mail: nkrao@iiap.res.in, E-mail: dll@astro.as.utexas.edu, E-mail: agarcia@iac.es [Physics Department, University of Nebraska at Omaha, NE 68182-0266 (United States)

    2012-11-20T23:59:59.000Z

    The remarkable hot R Coronae Borealis (RCB) star DY Cen is revealed to be the first and only binary system to be found among the RCB stars and their likely relatives, including the extreme helium stars and the hydrogen-deficient carbon stars. Radial velocity determinations from 1982 to 2010 have shown that DY Cen is a single-lined spectroscopic binary in an eccentric orbit with a period of 39.67 days. It is also one of the hottest and most H-rich member of the class of RCB stars. The system may have evolved from a common envelope to its current form.

  2. Search for Gravitational Waves from Compact Binary Coalescence in LIGO and Virgo Data from S5 and VSR1

    E-Print Network [OSTI]

    the LIGO Scientific Collaboration; the Virgo Collaboration

    2010-05-25T23:59:59.000Z

    We report the results of the first search for gravitational waves from compact binary coalescence using data from the LIGO and Virgo detectors. Five months of data were collected during the concurrent S5 (LIGO) and VSR1 (Virgo) science runs. The search focused on signals from binary mergers with a total mass between 2 and 35 Msun. No gravitational waves are identified. The cumulative 90%-confidence upper limits on the rate of compact binary coalescence are calculated for non-spinning binary neutron stars, black hole-neutron star systems, and binary black holes to be 8.7x10^-3, 2.2x10^-3 and 4.4x10^-4 yr^-1 L_10^-1 respectively, where L_10 is 10^10 times the blue solar luminosity. These upper limits are compared with astrophysical expectations.

  3. Clustering Binary Data Streams with K-means Carlos Ordonez

    E-Print Network [OSTI]

    Ordonez, Carlos

    .23 10 : notebook 0.02 0.56 0.45 0.07 11 : oil 0.21 0.11 0.56 0.70 12 : produce 0.43 0.05 0.82 0.21 13% 90-100%: meat 80-90%: bread 70-80%: oil {bread magazine } Table 1: Transaction clusters summary table of cutoff points and a number of top outliers per cluster. These cutoff points uniformly parti- tion

  4. Relativistic theory of tidal Love numbers

    E-Print Network [OSTI]

    Taylor Binnington; Eric Poisson

    2009-09-16T23:59:59.000Z

    In Newtonian gravitational theory, a tidal Love number relates the mass multipole moment created by tidal forces on a spherical body to the applied tidal field. The Love number is dimensionless, and it encodes information about the body's internal structure. We present a relativistic theory of Love numbers, which applies to compact bodies with strong internal gravities; the theory extends and completes a recent work by Flanagan and Hinderer, which revealed that the tidal Love number of a neutron star can be measured by Earth-based gravitational-wave detectors. We consider a spherical body deformed by an external tidal field, and provide precise and meaningful definitions for electric-type and magnetic-type Love numbers; and these are computed for polytropic equations of state. The theory applies to black holes as well, and we find that the relativistic Love numbers of a nonrotating black hole are all zero.

  5. What can SimbolX do for gammaray binaries? B. Cerutti, G. Dubus, G. Henri, A. B. Hill and A. Szostek

    E-Print Network [OSTI]

    Recanati, Catherine

    . Particles in gamma­ray binaries are accelerated with high efficiency to several TeV energiesWhat can Simbol­X do for gamma­ray binaries? B. Cerutti, G. Dubus, G. Henri, A. B. Hill and A Grenoble, France Abstract. Gamma­ray binaries have been uncovered as a new class of Galactic objects

  6. Robust high-contrast companion detection from interferometric observations. The CANDID algorithm and an application to six binary Cepheids

    E-Print Network [OSTI]

    Gallenne, A; Kervella, P; Monnier, J D; Schaefer, G H; Baron, F; Breitfelder, J; Bouquin, J B Le; Roettenbacher, R M; Gieren, W; Pietrzynski, G; McAlister, H; Brummelaar, T ten; Sturmann, J; Sturmann, L; Turner, N; Ridgway, S; Kraus, S

    2015-01-01T23:59:59.000Z

    Long-baseline interferometry is an important technique to spatially resolve binary or multiple systems in close orbits. By combining several telescopes together and spectrally dispersing the light, it is possible to detect faint components around bright stars. Aims. We provide a rigorous and detailed method to search for high-contrast companions around stars, determine the detection level, and estimate the dynamic range from interferometric observations. We developed the code CANDID (Companion Analysis and Non-Detection in Interferometric Data), a set of Python tools that allows us to search systematically for point-source, high-contrast companions and estimate the detection limit. The search pro- cedure is made on a N x N grid of fit, whose minimum needed resolution is estimated a posteriori. It includes a tool to estimate the detection level of the companion in the number of sigmas. The code CANDID also incorporates a robust method to set a 3{\\sigma} detection limit on the flux ratio, which is based on an a...

  7. Calibration of the modulation transfer function of surface profilometers with binary pseudo-random test standards: expanding the application range

    SciTech Connect (OSTI)

    Yashchuk, Valeriy V.; Anderson, Erik H.; Barber, Samuel K.; Bouet, Nathalie; Cambie, Rossana; Conley, Raymond; McKinney, Wayne R.; Takacs, Peter Z.; Voronov, Dmitriy L.

    2011-03-14T23:59:59.000Z

    A modulation transfer function (MTF) calibration method based on binary pseudo-random (BPR) gratings and arrays [Proc. SPIE 7077-7 (2007), Opt. Eng. 47, 073602 (2008)] has been proven to be an effective MTF calibration method for a number of interferometric microscopes and a scatterometer [Nucl. Instr. and Meth. A616, 172 (2010)]. Here we report on a further expansion of the application range of the method. We describe the MTF calibration of a 6 inch phase shifting Fizeau interferometer. Beyond providing a direct measurement of the interferometer's MTF, tests with a BPR array surface have revealed an asymmetry in the instrument's data processing algorithm that fundamentally limits its bandwidth. Moreover, the tests have illustrated the effects of the instrument's detrending and filtering procedures on power spectral density measurements. The details of the development of a BPR test sample suitable for calibration of scanning and transmission electron microscopes are also presented. Such a test sample is realized as a multilayer structure with the layer thicknesses of two materials corresponding to BPR sequence. The investigations confirm the universal character of the method that makes it applicable to a large variety of metrology instrumentation with spatial wavelength bandwidths from a few nanometers to hundreds of millimeters.

  8. Predicting landfalling hurricane numbers from basin hurricane numbers: basic statistical analysis

    E-Print Network [OSTI]

    Laepple, T; Penzer, J; Bellone, E; Nzerem, K; Laepple, Thomas; Jewson, Stephen; Penzer, Jeremy; Bellone, Enrica; Nzerem, Kechi

    2007-01-01T23:59:59.000Z

    One possible method for predicting landfalling hurricane numbers is to first predict the number of hurricanes in the basin and then convert that prediction to a prediction of landfalling hurricane numbers using an estimated proportion. Should this work better than just predicting landfalling hurricane numbers directly? We perform a basic statistical analysis of this question in the context of a simple abstract model.

  9. REFINED BOUNDS ON THE NUMBER OF CONNECTED ...

    E-Print Network [OSTI]

    2011-04-06T23:59:59.000Z

    Apr 6, 2011 ... Smith inequality (see Theorem 2.5) a bound on the number of semi- ... then using Smith inequality, have been used before in several different ...

  10. Harmonic resolution as a holographic quantum number

    E-Print Network [OSTI]

    Bousso, Raphael

    2009-01-01T23:59:59.000Z

    LBNL- 57239 Harmonic resolution as a holographic quantumhep-th/0310223 UCB-PTH-03/26 Harmonic resolution as aquantum number, the harmonic resolution K. The Bekenstein

  11. On Conformal Field Theory and Number Theory

    E-Print Network [OSTI]

    Huang, An

    2011-01-01T23:59:59.000Z

    Frontiers in Number Theory, Physics, and Ge- ometry II. (Witten, Quantum Field Theory, Crassmannians, and AlgebraicJ. Polchinski, String Theory, Vol. 1, Cambridge Univ.

  12. The Light Curve Variations of The Active Binaries With Hot Subdwarf Component

    E-Print Network [OSTI]

    Esin Sipahi; Serdar Evren

    2006-07-10T23:59:59.000Z

    We present the light curve variations of the two active binaries with hot subdwarf component. According to the brightness variations outside of the eclipses, the giant components of the systems are chromospherically active stars. The dark and cool active structures on this components cause the variations of the total light of the systems.

  13. Lifting Rationality Assumptions in Binary Aggregation Umberto Grandi and Ulle Endriss

    E-Print Network [OSTI]

    Endriss, Ulle

    Lifting Rationality Assumptions in Binary Aggregation Umberto Grandi and Ulle Endriss Institute aggregation procedure will lift the rationality assumptions from the in- dividual to the collective level, i an axiomatic characterisation of the class of aggregation proce- dures that will lift all rationality

  14. Computing Weight Distributions of Binary Linear Block Codes on a CCM ?

    E-Print Network [OSTI]

    Weinhardt, Markus

    Computing Weight Distributions of Binary Linear Block Codes on a CCM ? Markus Weinhardt Universit codes on an FPGA­based Custom Computing Machine (CCM). It consists of a heavily pipelined circuit­ plementation on a CCM, and section 4 reports on the performance of this im­ plementation. Finally, section 5

  15. SUPERORBITAL MODULATION OF X-RAY EMISSION FROM GAMMA-RAY BINARY LSI +61 303

    SciTech Connect (OSTI)

    Chernyakova, M. [School of Physical Sciences, Dublin City University, Glasnevin, Dublin 9 (Ireland); Neronov, A. [ISDC Data Center for Astrophysics, Chemin d'Ecogia 16, 1290 Versoix (Switzerland); Molkov, S.; Lutovinov, A. [Space Research Institute (IKI), 84/32 Profsoyuznaya Str., Moscow 117997 (Russian Federation); Malyshev, D. [Bogolyubov Institute for Theoretical Physics, 14-b Metrolohichna Street, Kiev 03680 (Ukraine); Pooley, G. [Astrophysics, Cavendish Laboratory, Cambridge CB3 0HE (United Kingdom)

    2012-03-10T23:59:59.000Z

    We report the discovery of a systematic constant time lag between the X-ray and radio flares of the gamma-ray binary LSI +61 303, persistent over a long, multi-year timescale. Using the data from the monitoring of the system by RXTE we show that the orbital phase of X-ray flares from the source varies from {phi}{sub X} {approx_equal} 0.35 to {phi}{sub X} {approx_equal} 0.75 on the superorbital 4.6 yr timescale. Simultaneous radio observations show that periodic radio flares always lag the X-ray flare by {Delta}{phi}{sub X-R} {approx_equal} 0.2. We propose that the constant phase lag corresponds to the time of flight of the high-energy particle-filled plasma blobs from inside the binary to the radio emission region at the distance of {approx}10 times the binary separation distance. We put forward a hypothesis that the X-ray bursts correspond to the moments of formation of plasma blobs inside the binary system.

  16. Short gamma-ray bursts from binary neutron star mergers in globular clusters

    E-Print Network [OSTI]

    Loss, Daniel

    ARTICLES Short gamma-ray bursts from binary neutron star mergers in globular clusters JONATHAN@cfa.harvard.edu Published online: 29 January 2006; doi:10.1038/nphys214 Observations by the Swift gamma-ray-burst (GRB, the so-called `long' GRBs (>2-200 s) were located by coded aperture imaging of their hard X-ray emission

  17. DEEP MULTI-TELESCOPE PHOTOMETRY OF NGC 5466. I. BLUE STRAGGLERS AND BINARY SYSTEMS

    SciTech Connect (OSTI)

    Beccari, G. [European Southern Observatory, Alonso de Cordova 3107, 19001 Santiago de Chile (Chile); Dalessandro, E.; Lanzoni, B.; Ferraro, F. R.; Miocchi, P. [Dipartimento di Fisica e Astronomia, Università degli Studi di Bologna, via Ranzani 1, I-40127 Bologna (Italy); Sollima, A.; Bellazzini, M., E-mail: gbeccari@eso.org [INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna (Italy)

    2013-10-10T23:59:59.000Z

    We present a detailed investigation of the radial distribution of blue straggler star (BSS) and binary populations in the Galactic globular cluster NGC 5466, over the entire extension of the system. We used a combination of data acquired with the Advanced Camera for Survey on board the Hubble Space Telescope, the LBC-blue mounted on the Large Binocular Telescope, and MEGACAM on the Canada-France-Hawaii Telescope. BSSs show a bimodal distribution with a mild central peak and a quite internal minimum. This feature is interpreted in terms of a relatively young dynamical age in the framework of the 'dynamical clock' concept proposed by Ferraro et al. The estimated fraction of binaries is ?6%-7% in the central region (r < 90'') and slightly lower (?5.5%) in the outskirts, at r > 200''. Quite interestingly, the comparison with the results of Milone et al. suggests that binary systems may also display a bimodal radial distribution, with the position of the minimum consistent with that of BSSs. If confirmed, this feature would give additional support to the scenario where the radial distribution of objects more massive than the average cluster stars is primarily shaped by the effect of dynamical friction. Moreover, this would also be consistent with the idea that the unperturbed evolution of primordial binaries could be the dominant BSS formation process in low-density environments.

  18. Eddy Current Tomography Using a Binary Markov Mila Nikolova and Ali MohammadDjafari

    E-Print Network [OSTI]

    Nikolova, Mila

    Eddy Current Tomography Using a Binary Markov Model Mila Nikolova and Ali Mohammad and notches. The medium is illuminated with a monochromatic electric field; the anomalies induce eddy currents in various fields such as nuclear power plants and aerospace engineering. 1 #12; The objective of eddy

  19. Rao-Blackwellization for Bayesian Variable Selection and Model Averaging in Linear and Binary Regression

    E-Print Network [OSTI]

    West, Mike

    of covariates to use in regression or generalized linear models is a ubiquitous problem. The Bayesian paradigm regression and binary re- gression with non-orthogonal design matrices in conjunction with independent "spike and kernel regression (Clyde and George 2004). The generalization of the Gaussian linear model to other

  20. acetonitrile-water binary mixtures: Topics by E-print Network

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    acetonitrile-water binary mixtures First Page Previous Page 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 Next Page Last Page Topic Index 1 Sudden structural...

  1. Simulation of Stresses during Casting of Binary Magnesium-Aluminum Alloys

    E-Print Network [OSTI]

    Beckermann, Christoph

    Simulation of Stresses during Casting of Binary Magnesium-Aluminum Alloys M.G. POKORNY, C.A. MONROE made for aluminum alloys.[6­8] Recently, Mathier and co-workers[9,10] performed a detailed com- parison between measured and predicted forces in the mush during solidification of dilute aluminum alloys

  2. Timing the Kilohertz Quasi-Periodic Oscillations in Low-mass X-ray Binaries

    E-Print Network [OSTI]

    Mariano Mendez

    2000-06-19T23:59:59.000Z

    I describe a new technique that we have been using in the past few years to get precise measurements of the frequency separation of the kHz QPOs in some Low-mass X-ray binaries. I show how this technique (that we call "shift-and-add") works, and I present some of the results we obtained using it.

  3. Transient neutron star X-ray binaries with Simbol-X

    E-Print Network [OSTI]

    S. Campana

    2007-09-24T23:59:59.000Z

    We present a brief overview of test-bed observations on accreting neutron star binaries for the Simbol-X mission. We show that Simbol-X will provide unique observations able to disclose the physical mechanisms responsible for their high energy emission.

  4. Preferential Solvent Partitioning within Asphaltenic Aggregates Dissolved in Binary Solvent Mixtures

    E-Print Network [OSTI]

    Kilpatrick, Peter K.

    Preferential Solvent Partitioning within Asphaltenic Aggregates Dissolved in Binary SolventVised Manuscript ReceiVed December 9, 2006 The heaviest fraction of crude oils, asphaltenes, has been shown to play-assembled interfacially active asphaltenic aggregates. Thus, careful characterization of these aggregates is of great

  5. Slag Metal Reactions in Binary CaF2-Metal Oxide Welding Fluxes

    E-Print Network [OSTI]

    Eagar, Thomas W.

    ) Slag Metal Reactions in Binary CaF2-Metal Oxide Welding Fluxes Some otherwise chemically stable fluxes may decompose into suboxides in the presence of welding arcs, thereby providing higher levels of 0 2 in weld metal than those oxides which do not form suboxides ABSTRACT. The stability of metal

  6. Investigation of the highest occupied molecular orbital of propene by binary (e, 2e) spectroscopy

    E-Print Network [OSTI]

    Wang, Yayu

    shell binding energy spectra of propene with impact energies of 600 and 1200 eV by a binary (e, 2e momentum distributions calculated using Har- tree­Fock and density functional theory methods with various wave effects. Ó 2004 Elsevier B.V. All rights reserved. 1. Introduction Electron momentum spectroscopy

  7. Blazars and the emerging AGN/black hole X-ray binary paradigm

    E-Print Network [OSTI]

    P. Uttley

    2005-08-02T23:59:59.000Z

    We briefly review the emerging paradigm which links the radio-quiet and radio-loud classes of AGN to the different accretion states observed in stellar mass black hole X-ray binary systems (BHXRBs), and discuss the relevance of the AGN/BHXRB connection to blazar variability.

  8. CS220 Spring 2014 Lab Assignment L3: Defusing a Binary Bomb

    E-Print Network [OSTI]

    Abu-Ghazaleh, Nael B.

    person for this lab. 1 Introduction The nefarious Dr. Evil has planted a slew of "binary bombs" on our machines (any of the machines in the G7 lab, or the LNG210 lab.) This includes the remote machines (remote you defuse your bomb. Please look at the hints section for some tips and ideas. The best way is to use

  9. Use of gravitational waves to measure alignment of spins in compact binaries

    E-Print Network [OSTI]

    Vitale, Salvatore; Graff, Philip; Sturani, Riccardo

    2015-01-01T23:59:59.000Z

    Coalescences of compact objects, neutron star and black holes, in binary systems are very promising sources of gravitational waves for the ground based detectors Advanced LIGO and Virgo. Much about compact binaries is still uncertain, including how often they are formed in the Universe, and some key details about their formation channels. One of the key open questions about compact binary coalescences is whether or not common envelope evolution is highly efficient in aligning spins with the orbital angular momentum. In this paper we show how gravitational waves detected by Advanced LIGO and Virgo can be used to verify if spins are preferentially aligned with the orbital angular momentum in compact binaries made of two black holes or a neutron star and a black hole. We first assume that all sources have either nearly aligned or non-aligned spins and use Bayesian model selection to calculate a cumulative odds ratio to compare the aligned and non-aligned models. We see that the correct model is typically preferr...

  10. Infrared Spectroscopy of the Ultra Low Mass Binary Oph 162225-240515

    E-Print Network [OSTI]

    Alexis Brandeker; Ray Jayawardhana; Valentin D. Ivanov; Radostin Kurtev

    2006-10-19T23:59:59.000Z

    Binary properties are an important diagnostic of the star and brown dwarf formation processes. While wide binaries appear to be rare in the sub-stellar regime, recent observations have revealed Ophiuchus 162225-240515 (2MASS J16222521-2405139) as a likely young ultra-low-mass binary with an apparent separation of ~240 AU. Here, we present low-resolution near-infrared spectra of the pair from NTT/SOFI (R~600) and VLT/ISAAC (R~1400), covering the 1.0-2.5um spectral region. By comparing to model atmospheres from Chabrier & Baraffe and Burrows et al., we confirm the surface temperatures to be T_A = (2350+/-150) K and T_B = (2100+/-100) K for the two components of the binary, consistent with earlier estimates from optical spectra. Using gravity sensitive K I features, we find the surface gravity to be significantly lower than field dwarfs of the same spectral type, providing the best evidence so far that these objects are indeed young. However, we find that models are not sufficiently reliable to infer accurate ages/masses from surface gravity. Instead, we derive masses of M_A = 13 (+8/-4) M_J and M_B = 10 (+5/-4) M_J for the two objects using the well-constrained temperatures and assuming an age of 1-10 Myr, consistent with the full range of ages reported for the Oph region.

  11. Beam Test of a Large Area nonn Silicon Strip Detector with Fast Binary Readout Electronics

    E-Print Network [OSTI]

    Beam Test of a Large Area n­on­n Silicon Strip Detector with Fast Binary Readout Electronics Y test was carried out for the non­irradiated and the irradiated detector modules. Efficiency, noise occupancy and performance in the edge regions were analyzed using the beam test data. High efficiency

  12. X-ray spectroscopy of low-mass X-ray binaries

    E-Print Network [OSTI]

    Juett, Adrienne Marie, 1976-

    2004-01-01T23:59:59.000Z

    I present high-resolution X-ray grating spectroscopy of neutron stars in low-mass X-ray binaries (LMXBs) using instruments onboard the Chandra X-ray Observatory and the X-ray Multi-Mirror Mission (XMM-Newton). The first ...

  13. In vitro corrosion and biocompatibility of binary magnesium alloys Xuenan Gu a

    E-Print Network [OSTI]

    Zheng, Yufeng

    In vitro corrosion and biocompatibility of binary magnesium alloys Xuenan Gu a , Yufeng Zheng a Corrosion In vitro Cytotoxicity Hemocompatibility a b s t r a c t As bioabsorbable materials, magnesium was used as control. Their mechanical properties, corrosion properties and in vitro biocompatibilities

  14. Unaligned Binary Codes for Index Compression in Schema-Independent Text Retrieval Systems

    E-Print Network [OSTI]

    Waterloo, University of

    during index construction. Schema- independent indices have different characteristics than document unaligned codes. Thus, their more compact index represen- tation does not carry the cost of a substantiallyUnaligned Binary Codes for Index Compression in Schema-Independent Text Retrieval Systems Stefan B

  15. Advances in Electrical and Computer Engineering Abstract--The linear, binary, block codes with no equally

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    Advances in Electrical and Computer Engineering 1 Abstract-- The linear, binary, block codes block codes is proposed. These codes are seen as sources with memory and the information quantities H(S,X), H(S), H(X), H(X|S), H(S|X), I(S,X) are derived. On the base of these quantities, the code

  16. Beam Test of a Large Area nonn Silicon Strip Detector with Fast Binary Readout Electronics

    E-Print Network [OSTI]

    Beam Test of a Large Area n­on­n Silicon Strip Detector with Fast Binary Readout Electronics Y­sided detector for the readout, its fabrication is similar to a double­sided device, because the backside, which

  17. AN X-RAY AND OPTICAL LIGHT CURVE MODEL OF THE ECLIPSING SYMBIOTIC BINARY SMC3

    SciTech Connect (OSTI)

    Kato, Mariko [Department of Astronomy, Keio University, Hiyoshi, Yokohama 223-8521 (Japan)] [Department of Astronomy, Keio University, Hiyoshi, Yokohama 223-8521 (Japan); Hachisu, Izumi [Department of Earth Science and Astronomy, College of Arts and Sciences, University of Tokyo, Komaba, Meguro-ku, Tokyo 153-8902 (Japan)] [Department of Earth Science and Astronomy, College of Arts and Sciences, University of Tokyo, Komaba, Meguro-ku, Tokyo 153-8902 (Japan); Mikolajewska, Joanna, E-mail: mariko@educ.cc.keio.ac.jp [Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716 Warszawa (Poland)] [Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716 Warszawa (Poland)

    2013-01-20T23:59:59.000Z

    Some binary evolution scenarios for Type Ia supernovae (SNe Ia) include long-period binaries that evolve to symbiotic supersoft X-ray sources in their late stage of evolution. However, symbiotic stars with steady hydrogen burning on the white dwarf's (WD) surface are very rare, and the X-ray characteristics are not well known. SMC3 is one such rare example and a key object for understanding the evolution of symbiotic stars to SNe Ia. SMC3 is an eclipsing symbiotic binary, consisting of a massive WD and red giant (RG), with an orbital period of 4.5 years in the Small Magellanic Cloud. The long-term V light curve variations are reproduced as orbital variations in the irradiated RG, whose atmosphere fills its Roche lobe, thus supporting the idea that the RG supplies matter to the WD at rates high enough to maintain steady hydrogen burning on the WD. We also present an eclipse model in which an X-ray-emitting region around the WD is almost totally occulted by the RG swelling over the Roche lobe on the trailing side, although it is always partly obscured by a long spiral tail of neutral hydrogen surrounding the binary in the orbital plane.

  18. A Low-Power Correlation Detector For Binary FSK Direct-Conversion Receivers

    E-Print Network [OSTI]

    Arslan, Hüseyin

    A Low-Power Correlation Detector For Binary FSK Direct-Conversion Receivers J. Min, H-C. Liu, A detector, Tone detection, Correlation, Direct-conversion wireless receivers Abstract A multiplierless-suited for low-power direct-conversion receivers used in wireless communications systems employ- ing FSK

  19. Black-Box Identification for PLC based MPC of a Binary Distillation Column

    E-Print Network [OSTI]

    Black-Box Identification for PLC based MPC of a Binary Distillation Column B. Huyck ,, F. Logist J is to upgrade the control system with a linear MPC running on a PLC. However, before a model based controller can be used on a PLC, an accurate (but simple) process model has to be constructed. Hence, the aim

  20. Quantum mechanical method of fragment's angular and energy distribution calculation for binary and ternary fission

    SciTech Connect (OSTI)

    Kadmensky, S. G., E-mail: kadmensky@phys.vsu.ru; Titova, L. V.; Pen'kov, N. V. [Voronezh State University (Russian Federation)

    2006-08-15T23:59:59.000Z

    In the framework of quantum-mechanical fission theory, the method of calculation for partial fission width amplitudes and asymptotic behavior of the fissile nucleus wave function with strong channel coupling taken into account has been suggested. The method allows one to solve the calculation problem of angular and energy distribution countation for binary and ternary fission.

  1. Evaluation of Hybrid Air-Cooled Flash/Binary Power Cycle

    SciTech Connect (OSTI)

    Greg Mines

    2005-10-01T23:59:59.000Z

    Geothermal binary power plants reject a significant portion of the heat removed from the geothermal fluid. Because of the relatively low temperature of the heat source (geothermal fluid), the performance of these plants is quite sensitive to the sink temperature to which heat is rejected. This is particularly true of air-cooled binary plants. Recent efforts by the geothermal industry have examined the potential to evaporatively cool the air entering the air-cooled condensers during the hotter portions of a summer day. While the work has shown the benefit of this concept, air-cooled binary plants are typically located in regions that lack an adequate supply of clean water for use in this evaporative cooling. In the work presented, this water issue is addressed by pre-flashing the geothermal fluid to produce a clean condensate that can be utilized during the hotter portions of the year to evaporatively cool the air. This study examines both the impact of this pre-flash on the performance of the binary plant, and the increase in power output due to the ability to incorporate an evaporative component to the heat rejection process.

  2. Simulator-analyzer for binary-cycle geothermal power plants: Volume 1, Executive summary: Final report

    SciTech Connect (OSTI)

    Greenlee, T.L.

    1987-04-01T23:59:59.000Z

    The object was to develop a generic dynamic simulator/analyzer for binary-cycle geothermal power plants for use on today's personal computers. The simulator/analyzer, as developed, can be used for (1) engineering analyses of static/dynamic performance and design trade-offs; (2) operator training and operating procedure evaluation; and (3) binary cycle technology demonstration. The simulator/analyzer consists of a set of ordinary non-linear differential equations that are programmed in a simulation language format and solved on an IBM-PC-AT. The equations are driven in an interactive mode by inputs from the PC keyboard and responses of plant temperatures, pressures, flows, etc., can be observed on a real-time color display that replicates a control room interface. Simulation predictions have been validated by comparisons with actual transient and steady state data taken from the Heber Binary Project, a 46.6 MWe binary-cycle demonstration power plant in operation in southern California. The simulation is accurate to within the uncertainty of the plant's process sensors. During this plant's later phases of construction, startup and operation, the simulator/analyzer is being used to: develop tuning constants for the Honeywell TDC-2000 control system, confirm failure/safety analyses study results, and support analyses of major operating events. It represents an adaptable tool for utilities and others involved in developing geothermal power generation facilities.

  3. ASIP-Based Multiprocessor SoC Design for Simple and Double Binary Turbo Decoding

    E-Print Network [OSTI]

    Muller, Olivier

    ASIP-Based Multiprocessor SoC Design for Simple and Double Binary Turbo Decoding Olivier Muller presents a new multiprocessor platform for high throughput turbo decoding. The proposed platform is based the recent shuffling technique introduced in the turbo-decoding field to reduce communication latency

  4. Tidal disruptions in circumbinary discs (I): Star formation, dynamics, and binary evolution

    E-Print Network [OSTI]

    Pau Amaro-Seoane; Patrick Brem; Jorge Cuadra

    2012-12-11T23:59:59.000Z

    In our current interpretation of the hierarchical structure of the universe it is well established that galaxies collide and merge with each other during their lifetime. If massive black holes (MBHs) reside in galactic centres, we expect them to form binaries in galactic nuclei surrounded by a circumbinary disc. If cooling is efficient enough, the gas in the disc will clump and trigger stellar formation in situ. In this first paper we address the evolution of the binary under the influence of the newly formed stars, which form individually and also clustered. We use SPH techniques to evolve the gas in the circumbinary disc and to study the phase of star formation. When the amount of gas in the disc is negligible, we further evolve the system with a high-accurate direct-summation $N-$body code to follow the evolution of the stars, the innermost binary and tidal disruption events (TDEs). For this, we modify the direct N-body code to (i) include treatment of TDEs and to (ii) include "gas cloud particles" that mimic the gas, so that the stellar clusters do not disolve when we follow their infall on to the MBHs. We find that the amount of stars disrupted by either infalling stellar clusters or individual stars is as large as 10^{-4}/yr per binary, higher than expected for typical galaxies.

  5. Binary inorganic salt mixtures as high conductivity liquid electrolytes for .100 uC fuel cells{

    E-Print Network [OSTI]

    Angell, C. Austen

    Binary inorganic salt mixtures as high conductivity liquid electrolytes for .100 uC fuel cells cations (e.g. ammonium) as electrolytes in fuel cells operating in the temperature range 100­200 uC, where cell operating with optimized electrodes in the same temperature range, while open circuit voltages

  6. Henry's law, surface tension, and surface adsorption in dilute binary mixtures

    E-Print Network [OSTI]

    Henry's law, surface tension, and surface adsorption in dilute binary mixtures Akira Onukia. The solute partitioning between gas and liquid Henry's law and the surface tension change are discussed fraction X and the temperature-derivative / T cx,p of the surface tension at fixed pressure p

  7. The information content of gravitational wave harmonics in compact binary inspiral

    E-Print Network [OSTI]

    Ronald W. Hellings; Thomas A. Moore

    2002-07-25T23:59:59.000Z

    The nonlinear aspect of gravitational wave generation that produces power at harmonics of the orbital frequency, above the fundamental quadrupole frequency, is examined to see what information about the source is contained in these higher harmonics. We use an order (4/2) post-Newtonian expansion of the gravitational wave waveform of a binary system to model the signal seen in a spaceborne gravitational wave detector such as the proposed LISA detector. Covariance studies are then performed to determine the ultimate accuracy to be expected when the parameters of the source are fit to the received signal. We find three areas where the higher harmonics contribute crucial information that breaks degeneracies in the model and allows otherwise badly-correlated parameters to be separated and determined. First, we find that the position of a coalescing massive black hole binary in an ecliptic plane detector, such as OMEGA, is well-determined with the help of these harmonics. Second, we find that the individual masses of the stars in a chirping neutron star binary can be separated because of the mass dependence of the harmonic contributions to the wave. Finally, we note that supermassive black hole binaries, whose frequencies are too low to be seen in the detector sensitivity window for long, may still have their masses, distances, and positions determined since the information content of the higher harmonics compensates for the information lost when the orbit-induced modulation of the signal does not last long enough to be apparent in the data.

  8. First all-sky search for continuous gravitational waves from unknown sources in binary systems

    E-Print Network [OSTI]

    The LIGO Scientific Collaboration; the Virgo Collaboration; J. Aasi; B. P. Abbott; R. Abbott; T. Abbott; M. R. Abernathy; T. Accadia; F. Acernese; K. Ackley; C. Adams; T. Adams; P. Addesso; R. X. Adhikari; C. Affeldt; M. Agathos; N. Aggarwal; O. D. Aguiar; A. Ain; P. Ajith; A. Alemic; B. Allen; A. Allocca; D. Amariutei; M. Andersen; R. Anderson; S. B. Anderson; W. G. Anderson; K. Arai; M. C. Araya; C. Arceneaux; J. Areeda; S. M. Aston; P. Astone; P. Aufmuth; C. Aulbert; L. Austin; B. E. Aylott; S. Babak; P. T. Baker; G. Ballardin; S. W. Ballmer; J. C. Barayoga; M. Barbet; B. C. Barish; D. Barker; F. Barone; B. Barr; L. Barsotti; M. Barsuglia; M. A. Barton; I. Bartos; R. Bassiri; A. Basti; J. C. Batch; J. Bauchrowitz; Th. S. Bauer; B. Behnke; M. Bejger; M. G. Beker; C. Belczynski; A. S. Bell; C. Bell; G. Bergmann; D. Bersanetti; A. Bertolini; J. Betzwieser; P. T. Beyersdorf; I. A. Bilenko; G. Billingsley; J. Birch; S. Biscans; M. Bitossi; M. A. Bizouard; E. Black; J. K. Blackburn; L. Blackburn; D. Blair; S. Bloemen; M. Blom; O. Bock; T. P. Bodiya; M. Boer; G. Bogaert; C. Bogan; C. Bond; F. Bondu; L. Bonelli; R. Bonnand; R. Bork; M. Born; V. Boschi; Sukanta Bose; L. Bosi; C. Bradaschia; P. R. Brady; V. B. Braginsky; M. Branchesi; J. E. Brau; T. Briant; D. O. Bridges; A. Brillet; M. Brinkmann; V. Brisson; A. F. Brooks; D. A. Brown; D. D. Brown; F. Brückner; S. Buchman; T. Bulik; H. J. Bulten; A. Buonanno; R. Burman; D. Buskulic; C. Buy; L. Cadonati; G. Cagnoli; J. Calderón Bustillo; E. Calloni; J. B. Camp; P. Campsie; K. C. Cannon; B. Canuel; J. Cao; C. D. Capano; F. Carbognani; L. Carbone; S. Caride; A. Castiglia; S. Caudill; M. Cavaglià; F. Cavalier; R. Cavalieri; C. Celerier; G. Cella; C. Cepeda; E. Cesarini; R. Chakraborty; T. Chalermsongsak; S. J. Chamberlin; S. Chao; P. Charlton; E. Chassande-Mottin; X. Chen; Y. Chen; A. Chincarini; A. Chiummo; H. S. Cho; J. Chow; N. Christensen; Q. Chu; S. S. Y. Chua; S. Chung; G. Ciani; F. Clara; J. A. Clark; F. Cleva; E. Coccia; P. -F. Cohadon; A. Colla; C. Collette; M. Colombini; L. Cominsky; M. Constancio Jr.; A. Conte; D. Cook; T. R. Corbitt; M. Cordier; N. Cornish; A. Corpuz; A. Corsi; C. A. Costa; M. W. Coughlin; S. Coughlin; J. -P. Coulon; S. Countryman; P. Couvares; D. M. Coward; M. Cowart; D. C. Coyne; R. Coyne; K. Craig; J. D. E. Creighton; T. D. Creighton; S. G. Crowder; A. Cumming; L. Cunningham; E. Cuoco; K. Dahl; T. Dal Canton; M. Damjanic; S. L. Danilishin; S. D'Antonio; K. Danzmann; V. Dattilo; H. Daveloza; M. Davier; G. S. Davies; E. J. Daw; R. Day; T. Dayanga; G. Debreczeni; J. Degallaix; S. Deléglise; W. Del Pozzo; T. Denker; T. Dent; H. Dereli; V. Dergachev; R. De Rosa; R. T. DeRosa; R. DeSalvo; S. Dhurandhar; M. Díaz; L. Di Fiore; A. Di Lieto; I. Di Palma; A. Di Virgilio; A. Donath; F. Donovan; K. L. Dooley; S. Doravari; S. Dossa; R. Douglas; T. P. Downes; M. Drago; R. W. P. Drever; J. C. Driggers; Z. Du; S. Dwyer; T. Eberle; T. Edo; M. Edwards; A. Effler; H. Eggenstein; P. Ehrens; J. Eichholz; S. S. Eikenberry; G. Endr?czi; R. Essick; T. Etzel; M. Evans; T. Evans; M. Factourovich; V. Fafone; S. Fairhurst; Q. Fang; S. Farinon; B. Farr; W. M. Farr; M. Favata; H. Fehrmann; M. M. Fejer; D. Feldbaum; F. Feroz; I. Ferrante; F. Ferrini; F. Fidecaro; L. S. Finn; I. Fiori; R. P. Fisher; R. Flaminio; J. -D. Fournier; S. Franco; S. Frasca; F. Frasconi; M. Frede; Z. Frei; A. Freise; R. Frey; T. T. Fricke; P. Fritschel; V. V. Frolov; P. Fulda; M. Fyffe; J. Gair; L. Gammaitoni; S. Gaonkar; F. Garufi; N. Gehrels; G. Gemme; E. Genin; A. Gennai; S. Ghosh; J. A. Giaime; K. D. Giardina; A. Giazotto; C. Gill; J. Gleason; E. Goetz; R. Goetz; L. Gondan; G. González; N. Gordon; M. L. Gorodetsky; S. Gossan; S. Goßler; R. Gouaty; C. Gräf; P. B. Graff; M. Granata; A. Grant; S. Gras; C. Gray; R. J. S. Greenhalgh; A. M. Gretarsson; P. Groot; H. Grote; K. Grover; S. Grunewald; G. M. Guidi; C. Guido; K. Gushwa; E. K. Gustafson; R. Gustafson; D. Hammer; G. Hammond; M. Hanke; J. Hanks; C. Hanna; J. Hanson; J. Harms; G. M. Harry; I. W. Harry; E. D. Harstad; M. Hart; M. T. Hartman; C. -J. Haster; K. Haughian; A. Heidmann; M. Heintze; H. Heitmann; P. Hello; G. Hemming; M. Hendry; I. S. Heng; A. W. Heptonstall; M. Heurs; M. Hewitson; S. Hild; D. Hoak; K. A. Hodge; K. Holt; S. Hooper; P. Hopkins; D. J. Hosken; J. Hough; E. J. Howell; Y. Hu; E. Huerta; B. Hughey; S. Husa; S. H. Huttner; M. Huynh; T. Huynh-Dinh; D. R. Ingram; R. Inta; T. Isogai; A. Ivanov; B. R. Iyer; K. Izumi; M. Jacobson; E. James; H. Jang; P. Jaranowski; Y. Ji; F. Jiménez-Forteza; W. W. Johnson; D. I. Jones; R. Jones; R. J. G. Jonker; L. Ju; Haris K; P. Kalmus; V. Kalogera; S. Kandhasamy; G. Kang; J. B. Kanner; J. Karlen; M. Kasprzack; E. Katsavounidis; W. Katzman; H. Kaufer; K. Kawabe; F. Kawazoe; F. Kéfélian; G. M. Keiser; D. Keitel; D. B. Kelley; W. Kells; A. Khalaidovski

    2014-09-17T23:59:59.000Z

    We present the first results of an all-sky search for continuous gravitational waves from unknown spinning neutron stars in binary systems using LIGO and Virgo data. Using a specially developed analysis program, the TwoSpect algorithm, the search was carried out on data from the sixth LIGO Science Run and the second and third Virgo Science Runs. The search covers a range of frequencies from 20 Hz to 520 Hz, a range of orbital periods from 2 to ~2,254 h and a frequency- and period-dependent range of frequency modulation depths from 0.277 to 100 mHz. This corresponds to a range of projected semi-major axes of the orbit from ~0.6e-3 ls to ~6,500 ls assuming the orbit of the binary is circular. While no plausible candidate gravitational wave events survive the pipeline, upper limits are set on the analyzed data. The most sensitive 95% confidence upper limit obtained on gravitational wave strain is 2.3e-24 at 217 Hz, assuming the source waves are circularly polarized. Although this search has been optimized for circular binary orbits, the upper limits obtained remain valid for orbital eccentricities as large as 0.9. In addition, upper limits are placed on continuous gravitational wave emission from the low-mass x-ray binary Scorpius X-1 between 20 Hz and 57.25 Hz.

  9. Binary Interpolation Search for Solution Mapping on Broadcast and Ondemand Channels in a Mobile

    E-Print Network [OSTI]

    Chen, Ming-Syan

    Computing Environment Jiun­Long Huang, Wen­Chih Peng and Ming­Syan Chen Department of Electrical Engineering search problem. In light of the theoretical properties derived, we devise an algorithm based on binary power source, and the Permission to make digital or hard copies of all or part of this work for personal

  10. Surface phase behavior in binary polymer mixtures. III. Temperature dependence of surface enrichment and of wetting

    E-Print Network [OSTI]

    Klein, Jacob

    enrichment and of wetting A. Budkowski,a) F. Scheffold, and J. Klein Department of Materials and Interfaces model systems, surface enrichment from polymer blends has clear technological implications-same mixtures--surface enrichment characteristics of the air- surface preferred phases. In these binary pairs

  11. Grant Title: NIDCD PHASE I/II PRELIMINARY CLINICAL TRIALS IN COMMUNICATION DISORDERS Funding Opportunity Number: PAR-12-123. CFDA Number(s): 93.173.

    E-Print Network [OSTI]

    Farritor, Shane

    Opportunity Number: PAR-12-123. CFDA Number(s): 93.173. Agency/Department: National Institutes of Health (NIH

  12. Grant Title: AHRQ HEALTH SERVICES RESEARCH DEMONSTRATION AND DISSEMINATION GRANTS Funding Opportunity Number: PA-13-046. CFDA Number(s): 93.226.

    E-Print Network [OSTI]

    Farritor, Shane

    Opportunity Number: PA-13-046. CFDA Number(s): 93.226. Agency/Department: Department of Health and Human

  13. Grant Title: INTELLECTUAL AND DEVELOPMENTAL DISABILITIES RESEARCH CENTERS (P30) Funding Opportunity Number: RFA-HD-13-002. CFDA Number(s): 93.865.

    E-Print Network [OSTI]

    Farritor, Shane

    Number: RFA-HD-13-002. CFDA Number(s): 93.865. Agency/Department: Department of Health and Human Services

  14. Grant Title: RESEARCH ON PSYCHOPATHOLOGY IN INTELLECTUAL DISABILITIES (R01) Funding Opportunity Number: PA-12-219. CFDA Number(s): 93.242.

    E-Print Network [OSTI]

    Farritor, Shane

    Number: PA-12-219. CFDA Number(s): 93.242. Agency/Department: Department of Health and Human Services

  15. Grant Title: MENTAL HEALTH RESEARCH DISSERTATION GRANT TO INCREASE DIVERSITY (R36) Funding Opportunity Number: PAR-12-103. CFDA Number(s): 93.242.

    E-Print Network [OSTI]

    Farritor, Shane

    Opportunity Number: PAR-12-103. CFDA Number(s): 93.242. Agency/Department: Department of Health and Human

  16. Grant Title: RESEARCH GRANTS FOR PREVENTING VIOLENCE AND VIOLENCE-RELATED INJURY Funding Opportunity Number: RFA-CE-14-006. CFDA Number(s): 93.136.

    E-Print Network [OSTI]

    Farritor, Shane

    Opportunity Number: RFA-CE-14-006. CFDA Number(s): 93.136. Agency/Department: Centers for Disease Control

  17. Grant Title: BEHAVIORAL SCIENCE TRACK AWARD FOR RAPID TRANSITION (B/START) (R03) Funding Opportunity Number: PAR-12-251. CFDA Number(s): 93.279.

    E-Print Network [OSTI]

    Farritor, Shane

    Opportunity Number: PAR-12-251. CFDA Number(s): 93.279. Agency/Department: Department of Health and Human

  18. Grant Title: ARTS IN EDUCATION MODEL DEVELOPMENT AND DISSEMINATION PROGRAM Funding Opportunity Number: ED-GRANTS-022013-001. CFDA Number(s): 84.351D.

    E-Print Network [OSTI]

    Farritor, Shane

    Number: ED-GRANTS-022013-001. CFDA Number(s): 84.351D. Agency/Department: Department of Education, Office

  19. Accurate evolutions of inspiralling neutron-star binaries: Prompt and delayed collapse to a black hole

    SciTech Connect (OSTI)

    Baiotti, Luca [Graduate School of Arts and Sciences, University of Tokyo, Komaba, Meguro-ku, Tokyo, 153-8902 (Japan); Max-Planck-Institut fuer Gravitationsphysik, Albert-Einstein-Institut, Potsdam-Golm (Germany); Giacomazzo, Bruno [Max-Planck-Institut fuer Gravitationsphysik, Albert-Einstein-Institut, Potsdam-Golm (Germany); Rezzolla, Luciano [Max-Planck-Institut fuer Gravitationsphysik, Albert-Einstein-Institut, Potsdam-Golm (Germany); Department of Physics and Astronomy, Louisiana State University, Baton Rouge, Louisiana (United States); INFN, Department of Physics, University of Trieste, Trieste (Italy)

    2008-10-15T23:59:59.000Z

    Binary neutron-star systems represent primary sources for the gravitational-wave detectors that are presently operating or are close to being operating at the target sensitivities. We present a systematic investigation in full general relativity of the dynamics and gravitational-wave emission from binary neutron stars which inspiral and merge, producing a black hole surrounded by a torus. Our results represent the state of the art from several points of view: (i) We use high-resolution shock-capturing methods for the solution of the hydrodynamics equations and high-order finite-differencing techniques for the solution of the Einstein equations; (ii) We employ adaptive mesh-refinement techniques with 'moving boxes' that provide high-resolution around the orbiting stars; (iii) We use as initial data accurate solutions of the Einstein equations for a system of binary neutron stars in irrotational quasicircular orbits; (iv) We exploit the isolated-horizon formalism to measure the properties of the black holes produced in the merger; (v) Finally, we use two approaches, based either on gauge-invariant perturbations or on Weyl scalars, to calculate the gravitational waves emitted by the system. Within our idealized treatment of the matter, these techniques allow us to perform accurate evolutions on time scales never reported before (i.e. {approx}30 ms) and to provide the first complete description of the inspiral and merger of a neutron-star binary leading to the prompt or delayed formation of a black hole and to its ringdown. We consider either a polytropic equation of state or that of an ideal fluid and show that already with this idealized treatment a very interesting phenomenology can be described. In particular, we show that while higher-mass polytropic binaries lead to the prompt formation of a rapidly rotating black hole surrounded by a dense torus, lower-mass binaries give rise to a differentially rotating star, which undergoes large oscillations and emits large amounts of gravitational radiation. Eventually, also the hyper-massive neutron star collapses to a rotating black hole surrounded by a torus. Finally, we also show that the use of a nonisentropic equation of state leads to significantly different evolutions, giving rise to a delayed collapse also with high-mass binaries, as well as to a more intense emission of gravitational waves and to a geometrically thicker torus.

  20. 2001 TRAFFIC ZONE BOUNDARIES Zone Numbers

    E-Print Network [OSTI]

    Toronto, University of

    2001 TRAFFIC ZONE BOUNDARIES Zone Numbers & Detailed Definitions #12;2001 TRAFFIC ZONE BOUNDARIES of Toronto Joint Program in Transportation January 2003 #12;PREFACE This report presents the 2001 traffic zone numbers by local municipalities in the 2001 TTS survey area. The second part presents detailed

  1. Geometrical accumulations and computably enumerable real numbers

    E-Print Network [OSTI]

    Durand-Lose, Jérôme

    Geometrical accumulations and computably enumerable real numbers (extended abstract) J and space are continuous and accumulations can be devised to unlimitedly accelerate a computation with rational numbers for coordinates and speeds, the time of any accumulation is a c.e. (compu- tably

  2. SOCIAL SECURITY NUMBER AND NAME VERIFICATION

    E-Print Network [OSTI]

    Amin, S. Massoud

    SOCIAL SECURITY NUMBER AND NAME VERIFICATION Academic Year 2014­2015 *FA552-A* Please recycle. DIRECTIONS--You must verify your name and Social Security number for processing of your 2014­2015 Free Application for Federal Student Aid (FAFSA) to continue. Please attach a legible copy of your Social Security

  3. SOCIAL SECURITY NUMBER AND NAME VERIFICATION

    E-Print Network [OSTI]

    Amin, S. Massoud

    SOCIAL SECURITY NUMBER AND NAME VERIFICATION Academic Year 2013­2014 *FA552-A* Please recycle. DIRECTIONS--You must verify your name and Social Security number for processing of your 2013­2014 Free Application for Federal Student Aid (FAFSA) to continue. Please attach a legible copy of your Social Security

  4. Search for lepton-family-number nonconservation

    SciTech Connect (OSTI)

    Hoffman, C.M.

    1986-01-01T23:59:59.000Z

    A review of the status of lepton-family-number nonconservation is given. After a brief historical and theoretical discussion, a description of how experimental searches for lepton-family-number nonconservation are performed is presented. Finally, a summary of the results from past experiments and prospects for future experiments is given.

  5. Protocol Number: (IBC office use only)

    E-Print Network [OSTI]

    Asaithambi, Asai

    Protocol Number: (IBC office use only) 1 UNF Registration of Biosafety Level 2 (BSL-2) A-2 Form", describe the methods of inactivation. #12;Protocol Number: (IBC office use only) 2 10. Describe the mechanism for decontaminating lab waste prior to disposal. Yes No If "Yes", describe the methods

  6. A Thermodynamic Classification of Real Numbers

    E-Print Network [OSTI]

    Thomas Garrity

    2009-03-15T23:59:59.000Z

    A new classification scheme for real numbers is given, motivated by ideas from statistical mechanics in general and work of Knauf and of Fiala and Kleban in particular. Critical for this classification of a real number will be the Diophantine properties of its continued fraction expansion.

  7. enter part number BNC / RP-BNC

    E-Print Network [OSTI]

    Berns, Hans-Gerd

    enter part number Products 7/16 1.0/2.3 1.6/5.6 AFI AMC BNC / RP-BNC C FAKRA SMB FME HN MCX Mini ------- Product Search ------- Inventory Search Search Results for: 31-10152-RFX Results: 1 - 1 of 1 Part Number. All rights reserved. Copyright | Terms & Conditions | RF E-Mail Client | Contact Us | Amphenol

  8. Company number 5857955 Wellcome Trust Finance plc

    E-Print Network [OSTI]

    Rambaut, Andrew

    Company number 5857955 Wellcome Trust Finance plc Annual Report and Financial Statements Year ended 30 September 2012 #12;Company number 5857955 Wellcome Trust Finance plc Contents Page Directors Trust Finance plc Directors' Report for the year ended 30 September 2012 Report of the Directors

  9. Company number 5857955 Wellcome Trust Finance plc

    E-Print Network [OSTI]

    Rambaut, Andrew

    Company number 5857955 Wellcome Trust Finance plc Annual Report and Financial Statements Year ended 30 September 2013 #12;Company number 5857955 Wellcome Trust Finance plc Contents Page Directors Trust Finance plc Directors' Report For the year ended 30 September 2013 Report of the Directors

  10. Experimental Number Theory Part I : Tower Arithmetic

    E-Print Network [OSTI]

    Zeilberger, Doron

    Experimental Number Theory Part I : Tower Arithmetic by Edinah K. Gnang January 15, 2011 1 rooted trees, which we shall here refer to as towers. The bijection between numbers and towers provides by XXX = (xk)1kn , (1) a tower expansion ( or simply a tower ) over XXX is a finite product of iterated

  11. Compendium of Experimental Cetane Number Data

    SciTech Connect (OSTI)

    Murphy, M. J.; Taylor, J. D.; McCormick, R. L.

    2004-09-01T23:59:59.000Z

    In this report, we present a compilation of reported cetane numbers for pure chemical compounds. The compiled database contains cetane values for 299 pure compounds, including 156 hydrocarbons and 143 oxygenates. Cetane number is a relative ranking of fuels based on the amount of time between fuel injection and ignition. The cetane number is typically measured either in a combustion bomb or in a single-cylinder research engine. This report includes cetane values from several different measurement techniques - each of which has associated uncertainties. Additionally, many of the reported values are determined by measuring blending cetane numbers, which introduces significant error. In many cases, the measurement technique is not reported nor is there any discussion about the purity of the compounds. Nonetheless, the data in this report represent the best pure compound cetane number values available from the literature as of August 2004.

  12. PHOTOMETRIC PROPERTIES FOR SELECTED ALGOL-TYPE BINARIES. V. V1241 TAURI

    SciTech Connect (OSTI)

    Yang, Y.-G.; Dai, H.-F. [School of Physics and Electronic Information, Huaibei Normal University, 235000 Huaibei, Anhui Province (China); Zhang, X.-B.; Li, H.-L., E-mail: yygcn@163.com [National Astronomical Observatories, Chinese Academy of Sciences, 100012 Beijing (China)

    2012-11-01T23:59:59.000Z

    We present new photometry for the eclipsing binary V1241 Tau, which was obtained on six nights between 2011 December and 2012 January using the 85 cm telescope at the Xinglong station of the National Astronomical Observatories of China. By using the updated Wilson-Devinney code, photometric models with third lights were deduced from two sets of light curves. The result implies that V1241 Tau is an Algol-type near-contact binary (NCB), whose mass ratio and filling-out of the primary are q = 0.545 ({+-} 0.003) and f{sub 1} = 82.4% ({+-} 0.2%), respectively. Based on all available times of minimum light spanning over 80 yr, the O - C curve of V1241 Tau appears to show a quasi-sinusoidal oscillation, i.e., a light-time orbit. The modulated period and amplitude are P{sub mod} = 47.4 ({+-} 1.7) yr and A = 0.0087 ({+-} 0.0005) days, respectively. This kind of period variation may be more likely attributed to the light-time effect via a presence of an unseen third body. From an analysis of 23 Algol-type NCBs with EB-type light curves, we determine that the fill-out for the primary f{sub 1} will increase as the orbital period P decreases. With angular momentum loss, the orbit of the binary will shrink, which causes f{sub 1} to increase. The primary component finally fills its Roche lobe, and the binary evolves into contact configuration. Therefore, this kind of Algol-type NCB with EB-type light curves, such as V1241 Tau, may be a progenitor of the A-type W UMa binary.

  13. Excitation of oscillation modes by tides in close binaries: constraints on stellar and orbital parameters

    E-Print Network [OSTI]

    B. Willems

    2003-09-01T23:59:59.000Z

    The parameter space favourable for the resonant excitation of free oscillation modes by dynamic tides in close binary components is explored using qualitative considerations to estimate the order of magnitude of the tidal force and the frequency range covered by the tidally induced oscillations. The investigation is valid for slowly rotating stars with masses in the interval between 2 and 20 solar masses, and an evolutionary stage ranging from the beginning to the end of the main sequence. Oscillation modes with eigenfrequencies of the order of five times the inverse of the star's dynamical time scale - i.e. the lowest-order p-modes, the f-mode, and the lowest-order g-modes - are found to be outside the favourable parameter space since their resonant excitation requires orbital eccentricities that are too high for the binary to stay detached when the components pass through the periastron of their relative orbit. Resonances between dynamic tides and g-modes with frequencies of the order of half of the inverse of the star's dynamical time scale on the other hand are found to be favourable for orbital periods up to 200 times the star's dynamical time scale, provided that the binary mass ratio q is larger than 1/3 and the orbital eccentricity e is larger than approximately 0.25. This favourable range comes down to orbital periods of up to 5-12 days in the case of 2-20 solar mass zero-age main-sequence binary components, and orbital periods of up to 21-70 days in the case of terminal main-sequence binary components.

  14. Warping and tearing of misaligned circumbinary disks around eccentric SMBH binaries

    E-Print Network [OSTI]

    Kimitake Hayasaki; Bong Won Sohn; Atsuo T. Okazaki; Taehyun Jung; Guangyao Zhao; Tsuguya Naito

    2015-02-01T23:59:59.000Z

    We study the warping and tearing of a geometrically thin, non-self-gravitating disk surrounding binary supermassive black holes on an eccentric orbit. The circumbinary disk is significantly misaligned with the binary orbital plane, and is subject to the time-dependent tidal torques. In principle, such a disk is warped and precesses, and is torn into mutually misaligned rings in the region, where the tidal precession torques are stronger than the local viscous torques. We derive the tidal-warp and tearing radii of the misaligned circumbinary disks around eccentric SMBH binaries. We find that in disks with the viscosity parameter, alpha, larger than a critical value depending on the disk aspect ratio, the disk warping appears outside the tearing radius. This condition is expressed as alpha > sqrt{H/3r} for H/r ~material is likely to rapidly accrete onto SMBHs. In warped and torn disks, both the tidal-warp and the tearing radii most strongly depend on the binary semi-major axis, although they also mildly depend on the other orbital and disk parameters. This strong dependence enables us to estimate the semi-major axis, once the tidal warp or tearing radius is determined observationally: For the tidal warp radius of 0.1 pc, the semi-major axis is estimated to be ~10^{-2} pc for 10^7 Msun black hole with typical orbital and disk parameters. We also briefly discuss the possibility that central objects of observed warped maser disks in active galactic nuclei are supermassive black hole binaries.

  15. Evolution of binary black holes in self gravitating discs: dissecting the torques

    E-Print Network [OSTI]

    Constanze Roedig; Alberto Sesana; Massimo Dotti; Jorge Cuadra; Pau Amaro-Seoane; Francesco Haardt

    2012-08-14T23:59:59.000Z

    We study the interplay between gas accretion and gravity torques in changing a binary elements and its total angular momentum (L) budget. Especially, we analyse the physical origin of the gravity torques (T_g) and their location within the disc. We analyse 3D SPH simulations of the evolution of initially quasi-circular massive black hole binaries (BHBs) residing in the central hollow of massive self-gravitating circumbinary discs. We use different thermodynamics within the cavity and for the numerical size of the black holes to show that (i) the BHB eccentricity growth found previously is a general result, independent of the accretion and the adopted thermodynamics; (ii) the semi-major axis decay depends both on the T_g and on the interplay with the disc-binary L-transfer due to accretion; (iii) the spectral structure of the T_g is predominately caused by disc edge overdensities and spiral arms developing in the body of the disc and, in general, does not reflect directly the period of the binary; (iv) the net T_g changes sign across the BHB corotation radius. We quantify the relative importance of the two, which appear to depend on the thermodynamical properties of the instreaming gas, and which is crucial in assessing the disc-binary L-transfer; (v) the net torque manifests as a purely kinematic (non-resonant) effect as it stems from the cavity, where the material flows in and out in highly eccentric orbits. Both accretion onto the black holes and the interaction with gas streams inside the cavity must be taken into account to assess the fate of the BHB. Moreover, the total torque exerted by the disc affects L(BHB) by changing all the elements (mass, mass ratio, eccentricity, semimajor axis) of the BHB. Common prescriptions equating tidal torque to semi-major axis shrinking might therefore be poor approximations for real astrophysical systems.

  16. Isobaric vapor-liquid equilibria for binary and ternary systems composed of water, 1-propanol, and 2-propanol at 100 kPa

    SciTech Connect (OSTI)

    Gabaldon, C.; Marzal, P.; Monton, J.B.; Rodrigo, M.A. [Univ. de Valencia (Spain). Dept. de Ingenieria Quimica] [Univ. de Valencia (Spain). Dept. de Ingenieria Quimica

    1996-11-01T23:59:59.000Z

    Isobaric vapor-liquid equilibria data were obtained for the 2-propanol + 1-propanol binary system and the water + 1-propanol + 2-propanol ternary system at 100 kPa. The data were found to be thermodynamically consistent according to the Van Ness-Byer-Gibbs method for the binary system and according to the McDermott-Ellis method for the ternary one. The binary system is well represented by assuming ideal behavior. The binary interaction parameters obtained from this and previous work are used to predict the vapor-liquid equilibrium for the ternary system using the UNIQUAC, NRTL, and Wilson models. The ternary system is well predicted from binary data.

  17. Dynamics of stellar black holes in young star clusters with different metallicities - II. Black hole-black hole binaries

    E-Print Network [OSTI]

    Brunetto Marco Ziosi; Michela Mapelli; Marica Branchesi; Giuseppe Tormen

    2014-05-20T23:59:59.000Z

    In this paper, we study the formation and dynamical evolution of black hole-black hole (BH-BH) binaries in young star clusters (YSCs), by means of N-body simulations. The simulations include metallicity-dependent recipes for stellar evolution and stellar winds, and have been run for three different metallicities (Z = 0.01, 0.1 and 1 Zsun). Following recent theoretical models of wind mass-loss and core-collapse supernovae, we assume that the mass of the stellar remnants depends on the metallicity of the progenitor stars. We find that BH-BH binaries form efficiently because of dynamical exchanges: in our simulations, we find about 10 times more BH-BH binaries than double neutron star binaries. The simulated BH-BH binaries form earlier in metal-poor YSCs, which host more massive black holes (BHs) than in metal-rich YSCs. The simulated BH-BH binaries have very large chirp masses (up to 80 Msun), because the BH mass is assumed to depend on metallicity, and because BHs can grow in mass due to the merger with stars. The simulated BH-BH binaries span a wide range of orbital periods (10^-3-10^7 yr), and only a small fraction of them (0.3 per cent) is expected to merge within a Hubble time. We discuss the estimated merger rate from our simulations and the implications for Advanced VIRGO and LIGO.

  18. Grant Title: DECISION, RISK AND MANAGEMENT SCIENCES (DRMS) Funding Opportunity Number: PD-98-1321. CFDA Number(s): 47.075.

    E-Print Network [OSTI]

    Farritor, Shane

    -1321. CFDA Number(s): 47.075. Agency/Department: National Science Foundation. Area of Research: Research

  19. Grant Title: NIH DIRECTOR'S EARLY INDEPENDENCE AWARDS (DP5) Funding Opportunity Number: RFA-RM-12-018. CFDA Number(s): 93.310.

    E-Print Network [OSTI]

    Farritor, Shane

    -018. CFDA Number(s): 93.310. Agency/Department: Department of Health and Human Services, Office of Strategic

  20. Grant Title: NIDCD CLINICAL RESEARCH CENTER GRANT (P50) Funding Opportunity Number: PAR-13-277. CFDA Number(s): 93.173.

    E-Print Network [OSTI]

    Farritor, Shane

    -277. CFDA Number(s): 93.173. Agency/Department: National Institutes of Health (NIH), National Institute

  1. Grant Title: ACADEMIC-COMMUNITY PARTNERSHIP CONFERENCE SERIES (R13) Funding Opportunity Number: PAR-12-102. CFDA Number(s): 93.865.

    E-Print Network [OSTI]

    Farritor, Shane

    -12-102. CFDA Number(s): 93.865. Agency/Department: Department of Health and Human Services, National

  2. Grant Title: ALCOHOL RESEARCH EDUCATION PROJECT GRANTS (R25) Funding Opportunity Number: PAR -11-205. CFDA Number(s) 93.273.

    E-Print Network [OSTI]

    Farritor, Shane

    -205. CFDA Number(s) 93.273. Agency/Department: Department of Health and Human Services (HHS), National

  3. Grant Title: NIDA CORE CENTER OF EXCELLENCE GRANT PROGRAM (P30) Funding Opportunity Number: PAR-10-220. CFDA Number(s): 93.279.

    E-Print Network [OSTI]

    Farritor, Shane

    -220. CFDA Number(s): 93.279. Agency/Department: Department of Health and Human Services, National Institutes

  4. Grant Title: INITIATIVE FOR MAXIMIZING STUDENT DEVELOPMENT (IMSD) (R25) Funding Opportunity Number: PAR-13-082. CFDA Number(s): 93.859.

    E-Print Network [OSTI]

    Farritor, Shane

    : PAR-13-082. CFDA Number(s): 93.859. Agency/Department: National Institutes of Health (NIH), National

  5. ON THE PROBLEM OF UNIQUENESS FOR THE MAXIMUM STIRLING NUMBER(S) OF THE SECOND KIND

    E-Print Network [OSTI]

    Pomerance, Carl

    ON THE PROBLEM OF UNIQUENESS FOR THE MAXIMUM STIRLING NUMBER(S) OF THE SECOND KIND E. Rodney Say that an integer n is exceptional if the maximum Stirling number of the second kind S(n, k) occurs or equal to x is O(x3/5+ ), for any > 0. 1. Introduction Let S(n, k) be the Stirling number of the second

  6. OMB Control Number: 1910-5165

    Energy Savers [EERE]

    OMB Control Number: 1910-5165 Expires: xxxx201x SEMI-ANNUAL DAVIS-BACON ENFORCEMENT REPORT Please submit this Semi-Annual Davis-Bacon Enforcement Report to your site DOENNSA...

  7. Estimating visitor and visit numbers to

    E-Print Network [OSTI]

    ............................................ 24 4.5 Monitoring and Evaluating Quality of Life for CRS'07 .......................................25 4.6 Quality of experience visitor, visit and total numbers of visits to woodlands. This document builds on guidance on visitor

  8. REFINED BOUNDS ON THE NUMBER OF CONNECTED ...

    E-Print Network [OSTI]

    2011-11-06T23:59:59.000Z

    Nov 6, 2011 ... closure imply using the well-known Smith inequality (see Theorem 2.4) a bound on the number of semi-algebraically connected components of ...

  9. Libraries Reference Document Number: 253262-002

    E-Print Network [OSTI]

    Talbot, James P.

    Intel® Fortran Libraries Reference Document Number: 253262-002 World Wide Web: http PROPERTY RIGHT. Intel products are not intended for use in medical, life saving, or life sustain- ing.................................................................................... xxiv Chapter 1 Overview of the Libraries Portability Routines

  10. THE NEW ELEMENT BERKELIUM (ATOMIC NUMBER 97)

    E-Print Network [OSTI]

    Thompson, S.G.; Ghiorso, A.; Seaborg, G.T.

    2008-01-01T23:59:59.000Z

    NUMBER 97) Stanley G. Thompson, Albert Ghiorso, and Glenn T.Rev Eventually 5 S • G. Thompson, Physo Revo 76, 319 (1949)0~'Street, Ghiorso, and Thompson, unpublished work. UCRL-669

  11. CORAL Name: STS 1 Model Number: ICP

    E-Print Network [OSTI]

    Reif, Rafael

    CORAL Name: STS 1 Model Number: ICP Location: TRL What it does: Deep Silicon Etch Introduction prior to use and to ENGAGE MACHINE prior to starting your process in CORAL. Venting and Loading a Wafer

  12. Contributions to Metric Number Technical Report

    E-Print Network [OSTI]

    Dent, Alexander W.

    Contributions to Metric Number Theory Paul Rowe Technical Report RHUL­MA­2002­2 5 December 2002, Professor Glyn Harman, for sug- gestions of problems to attempt, helpful advice on methods and help

  13. Elastic tail propulsion at low Reynolds number

    E-Print Network [OSTI]

    Yu, Tony S. (Tony Sheung)

    2007-01-01T23:59:59.000Z

    A simple way to generate propulsion at low Reynolds number is to periodically oscillate a passive flexible filament. Here we present a macroscopic experimental investigation of such a propulsive mechanism. A robotic swimmer ...

  14. ARE Update Volume 6, Number 1

    E-Print Network [OSTI]

    Carter, Colin A.; Just, David; Zilberman, David; Karp, Larry

    2002-01-01T23:59:59.000Z

    in California, the major GM crop is cotton. However, biotechor impossible if the GM crop is highly pro- internationala small number of authorized GM crops in the EU. Partly in

  15. The concrete theory of numbers : Problem of simplicity of Fermat number-twins

    E-Print Network [OSTI]

    Boris V. Tarasov

    2007-07-06T23:59:59.000Z

    The problem of simplicity of Fermat number-twins $f_{n}^{\\pm}=2^{2^n}\\pm3$ is studied. The question for what $n$ numbers $f_{n}^{\\pm}$ are composite is investigated. The factor-identities for numbers of a kind $x^2 \\pm k $ are found.

  16. Sequence and Series of Real Numbers 1.1 Sequence of Real Numbers

    E-Print Network [OSTI]

    Nair, M.Thamban

    1 Sequence and Series of Real Numbers 1.1 Sequence of Real Numbers Suppose for each positive a sequence, and this ordered list is usually written as (a1, a2, . . . , . . .) or (an) or {an}. More precisely, we define a sequence as follows: Definition 1.1 A sequence of real numbers is a function from

  17. SESAME equation of state number 7740: Polycarbonate

    SciTech Connect (OSTI)

    Boettger, J.C.

    1991-06-01T23:59:59.000Z

    An equation of state (EOS) for polycarbonate (a widely used polymer) has been generated with the computer code GRIZZLY and will be added to the SESAME library as material number 7740. Although a number of the input parameter used in the calculations are based on rough estimates. 7740 provides a good match to experimental Hugoniot data and should be reliable on or near the principal Hugoniot. 6 refs., 1 fig.

  18. Dynamical real numbers and living systems

    E-Print Network [OSTI]

    Dhurjati Prasad Datta

    2010-01-11T23:59:59.000Z

    Recently uncovered second derivative discontinuous solutions of the simplest linear ordinary differential equation define not only an nonstandard extension of the framework of the ordinary calculus, but also provide a dynamical representation of the ordinary real number system. Every real number can be visualized as a living cell -like structure, endowed with a definite evolutionary arrow. We discuss the relevance of this extended calculus in the study of living systems. We also present an intelligent version of the Newton's first law of motion.

  19. Sensitivity comparison of searches for binary black hole coalescences with ground-based gravitational-wave detectors

    E-Print Network [OSTI]

    Mohapatra, Satya

    Searches for gravitational-wave transients from binary black hole coalescences typically rely on one of two approaches: matched filtering with templates and morphology-independent excess power searches. Multiple algorithmic ...

  20. Search for gravitational waves from compact binary coalescence in LIGO and Virgo data from S5 and VSR1

    E-Print Network [OSTI]

    Barsotti, Lisa

    We report the results of the first search for gravitational waves from compact binary coalescence using data from the Laser Interferometer Gravitational-Wave Observatory and Virgo detectors. Five months of data were collected ...