National Library of Energy BETA

Sample records for thrust belt prepared

  1. Grenville foreland thrust belt hidden beneath the eastern US midcontinent

    SciTech Connect (OSTI)

    Hauser, E.C. (Cornell Univ., Ithaca, NY (United States))

    1993-01-01

    Grenville foreland thrust structures are observed beneath the eastern US midcontinent on COCORP (Consortium for Continental Reflection Profiling) line OH-1 and a short seismic line in southwest Ohio. These structures represent the first evidence for a significant Grenville foreland thrust belt preserved in eastern North America. On the COCORP lines, the structures include a thrust ramp anticline and an associated asymmetric syncline. The Grenville front tectonic zone appears to truncate these foreland structures, indicating a later, second phase expressed as a deeply penetrating, out-of-sequence thrust zone associated with the main uplift of the Grenville province on the east. A short, shallow seismic line in southwestern Ohio reveals an east-dipping sequence of prominently layered rocks that may lie above a footwall ramp to a deeper Grenville thrust fault. A drill hole into the less reflective top of this dipping sequence encountered unmetamorphosed sedimentary rocks like those increasingly reported from other drill holes in southwestern Ohio and adjacent states. Although possibly part of a late Precambrian (Keweenawan ) rift, these clastic sedimentary rocks may instead preserve evidence of a heretofore unrecognized Grenville foreland basin in eastern North America. Alternatively these Precambrian sedimentary rocks together with an underlying, but yet undrilled, strongly layered sequence may correlate with similarly layered rocks observed on COCORP and industrial seismic lines within the Middle Proterozoic granite-rhyolite province to the west in Indiana and Illinois and indicate that unmetamorphosed sedimentary material is an important constituent of the granite-rhyolite province. 25 refs., 6 figs.

  2. Late Cenozoic partitioning of oblique plate convergence in the Zagros fold-and-thrust belt (Iran)

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    Late Cenozoic partitioning of oblique plate convergence in the Zagros fold-and-thrust belt (Iran 2 May 2006. [1] The NW trending Zagros fold-and-thrust belt is affected by two major dextral faults operating at the rear of the belt has become partitioned along the newly formed Main Recent Fault

  3. Structure and evolution of the active fold and thrust belt of southwestern Taiwan using GPS geodesy 

    E-Print Network [OSTI]

    Hickman, John Bibb

    1999-01-01

    Using GPS and published geologic data, we have crographics. investigated the current deformation rates and local kinematic relationships for the southern region of the Taiwan fold-thrust belt. The GPS measurements suggest complex motions across...

  4. Thrust belt architecture of the central and southern Western Foothills of Taiwan 

    E-Print Network [OSTI]

    Rodriguez-Roa, Fernando Antonio

    2009-05-15

    A structural model of the central and southern Western Foothills Fold and Thrust Belt (WFFTB) was constructed from serial balanced cross sections. The cross sections are constrained by published surface and subsurface geologic data...

  5. Deformation zone `jumps' in a young convergent setting; the Lengguru fold-and-thrust belt, New Guinea Island

    E-Print Network [OSTI]

    Nicolas, Chamot-Rooke

    Deformation zone `jumps' in a young convergent setting; the Lengguru fold-and-thrust belt, New The Lengguru fold-and-thrust belt in West Papua (Indonesia) has all the characteristics of a young orogen buttress. The construction of these two wedges is younger than 11 Myr. The structures of the Lengguru belt

  6. GEOLOGY | Volume 43 | Number 7 | www.gsapubs.org 1 Foreland basin stratigraphic control on thrust belt evolution

    E-Print Network [OSTI]

    Fay, Noah

    belt evolution James B. Chapman and Peter G. DeCelles Department of Geosciences, University of Arizona on thrust belt architecture have not been fully evalu- ated. Mechanical properties of typical foreland basin stratigraphic successions influence the structural development of fold-thrust belts in predictable ways

  7. Numerical investigation of deformation mechanics in fold-and-thrust belts: Influence of rheology

    E-Print Network [OSTI]

    Kaus, Boris

    -and-thrust belts related to convergence tectonics develop by scraping off a rock sequence along a weaker basal décollement often formed by water-saturated shale layers or low-viscosity salt horizons. A two friction angles as the cover sequence. Model salt layers behave linear viscous, due to a lower viscosity

  8. Fold and thrust partitioning in a contracting fold belt: Insights from the 1931 Mach earthquake in Baluchistan

    E-Print Network [OSTI]

    Bilham, Roger

    models of the earthquake cycle in this fold and thrust belt suggest that slip on the frontal thrust fault is $5 mm/yr. Hence the minimum renewal time between earthquakes with 1.2-m mean displacement should is taken into account the minimum renewal time may exceed 2000 years. Citation: Szeliga, W., R. Bilham, D

  9. The Cordilleran foreland thrust belt in northwestern Montana and northern Idaho from COCORP and industry seismic reflection data

    SciTech Connect (OSTI)

    Yoos, T.R.; Potter, C.J.; Thigpen, J.L.; Brown, L.D. (Cornell Univ., Ithaca, NY (United States))

    1991-06-01

    COCORP and petroleum industry seismic reflection profiles in northwestern Montana reveal the structure of the Cordilleran foreland thrust belt. The Front Ranges consist of thick thrust sheets containing Precambrian Belt Supergroup and Paleozoic miogeoclinal shelf rocks above a thin remnant of Paleozoic rocks and gently westward-dipping North American basement. Interpretation of the seismic data and results from a recent petroleum exploration well suggest that 15-22 km of Precambrian Belt Supergroup sedimentary rocks are present in several thrust plates beneath the eastern Purcell anticlinorium. Previous hypotheses of a large mass of Paleozoic miogeoclinal sedimentary rocks or slices of crystalline basement located beneath the eastern Purcell anticlinorium do not appear to be supported by the data. The easternmost occurrence of allochthonous basement is interpreted to be in the western part of the anticlinorium near the Montana-Idaho border. Comparison of the Cordilleran foreland thrust belt in northwestern Montana and southern Canada suggest that a change in the deep structure of the Purcell anticlinorium occurs along strike. The anticlinorium in southern Canada has been interpreted as a hanging-wall anticline that was thrust over the western edge of thick Proterozoic North American basement, whereas in northwestern Montana the anticlinorium appears to consist of a complex series of thrust sheets above highly attenuated North American basement.

  10. The vertical separation of mainshock rupture and microseismicity at Qeshm island in the Zagros fold-and-thrust belt, Iran

    E-Print Network [OSTI]

    Elliott, John

    -and-thrust belt, Iran E. Nissen a, , F. Yamini-Fard b , M. Tatar b , A. Gholamzadeh b,1 , E. Bergman c , J Engineering and Seismology, PO Box 19395-3913, Tehran, Iran c Department of Physics, University of Colorado rights reserved. 1. Introduction The Zagros mountains in south-western Iran are one of the most rapidly

  11. The Role of Climate in the Deformation of a Fold and Thrust Belt 

    E-Print Network [OSTI]

    Steen, Sean Kristian

    2012-02-14

    Theory and experiment show that the rate and geographic distribution of erosion control the rate and pattern of deformation in collisional mountain belts. Enhanced erosion reduces the mass of material that must be moved up and over ramps...

  12. Conditions during syntectonic vein formation in the footwall of the Absaroka thrust fault of the Idaho-Wyoming-Utah fold and thrust belt 

    E-Print Network [OSTI]

    Lambert, George Randall

    1993-01-01

    Results. . Isotope Thermometry . FRACTURE MECHANICS . Analysis Procedure and Results DISCUSSION . Thrust Faulting and Overburden Temperatures. Geothermal Gradient Constraints. Twtn Creek Formation Fluid Flow? Closed system. Open System. . tv vt...C. The lithostatic and hydrostatic thermobartc gradients were calculated using a 26 MPa/km hthostatic gradient, a 10 MPa/km hydrostatic gradient and a 25oC/km geothermal gradient. The present mean surface temperature in this portion of the Idaho-Wyoming-Utah fold...

  13. San Juan Montana Thrust Belt WY Thrust Belt Black Warrior

    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: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustments (Billion Cubic Feet) Wyoming963 1.969 1.979 1.988 1.996 2.003 1990-2016November 2000 Overview OilSan

  14. Measuring axial pump thrust

    DOE Patents [OSTI]

    Suchoza, B.P.; Becse, I.

    1988-11-08

    An apparatus for measuring the hydraulic axial thrust of a pump under operation conditions is disclosed. The axial thrust is determined by forcing the rotating impeller off of an associated thrust bearing by use of an elongate rod extending coaxially with the pump shaft. The elongate rod contacts an impeller retainer bolt where a bearing is provided. Suitable measuring devices measure when the rod moves to force the impeller off of the associated thrust bearing and the axial force exerted on the rod at that time. The elongate rod is preferably provided in a housing with a heat dissipation mechanism whereby the hot fluid does not affect the measuring devices. 1 fig.

  15. Measuring axial pump thrust

    DOE Patents [OSTI]

    Suchoza, Bernard P. (McMurray, PA); Becse, Imre (Washington, PA)

    1988-01-01

    An apparatus for measuring the hydraulic axial thrust of a pump under operation conditions is disclosed. The axial thrust is determined by forcing the rotating impeller off of an associated thrust bearing by use of an elongate rod extending coaxially with the pump shaft. The elongate rod contacts an impeller retainer bolt where a bearing is provided. Suitable measuring devices measure when the rod moves to force the impeller off of the associated thrust bearing and the axial force exerted on the rod at that time. The elongate rod is preferably provided in a housing with a heat dissipation mechanism whereby the hot fluid does not affect the measuring devices.

  16. Variable thrust cartridge

    DOE Patents [OSTI]

    Taleyarkhan, Rusi P. (Knoxville, TN)

    2000-11-07

    The present invention is a variable thrust cartridge comprising a water-molten aluminum reaction chamber from which a slug is propelled. The cartridge comprises a firing system that initiates a controlled explosion from the reaction chamber. The explosive force provides a thrust to a slug, preferably contained within the cartridge.

  17. A two-dimensional finite difference model of the effects of erosion on the evolution of pore pressure within a moving thrust sheet 

    E-Print Network [OSTI]

    Sales, James Gregory

    1994-01-01

    There is indirect for the existence of abnormal pore pressures in continental thrust belts. Workers have also shown through modeling studies that abnormal pore pressures are to be expected in tectonic wedges which have the physical properties...

  18. Laterally bendable belt conveyor

    DOE Patents [OSTI]

    Peterson, William J. (Coraopolis, PA)

    1985-01-01

    An endless, laterally flexible and bendable belt conveyor particularly adapted for coal mining applications in facilitating the transport of the extracted coal up- or downslope and around corners in a continuous manner is disclosed. The conveying means includes a flat rubber belt reinforced along the middle portion thereof along which the major portion of the belt tension is directed so as to cause rotation of the tubular shaped belt when trammed around lateral turns thus preventing excessive belt bulging distortion between adjacent belt supports which would inhibit belt transport. Pretension induced into the fabric reinforced flat rubber belt by conventional belt take-up means supports the load conveyed when the belt conveyor is making lateral turns. The carrying and return portions of the belt are supported and formed into a tubular shape by a plurality of shapers positioned along its length. Each shaper is supported from above by a monorail and includes clusters of idler rollers which support the belt. Additional cluster rollers in each shaper permit the belt supporting roller clusters to rotate in response to the belt's operating tension imposed upon the cluster rollers by induced lateral belt friction forces. The freely rotating roller clusters thus permit the belt to twist on lateral curves without damage to itself while precluding escape of the conveyed material by effectively enclosing it in the tube-shaped, inner belt transport length.

  19. Micro thrust and heat generator

    DOE Patents [OSTI]

    Garcia, E.J.

    1998-11-17

    A micro thrust and heat generator have a means for providing a combustion fuel source to an ignition chamber of the micro thrust and heat generator. The fuel is ignited by a ignition means within the micro thrust and heat generator`s ignition chamber where it burns and creates a pressure. A nozzle formed from the combustion chamber extends outward from the combustion chamber and tappers down to a narrow diameter and then opens into a wider diameter where the nozzle then terminates outside of said combustion chamber. The pressure created within the combustion chamber accelerates as it leaves the chamber through the nozzle resulting in pressure and heat escaping from the nozzle to the atmosphere outside the micro thrust and heat generator. The micro thrust and heat generator can be microfabricated from a variety of materials, e.g., of polysilicon, on one wafer using surface micromachining batch fabrication techniques or high aspect ratio micromachining techniques (LIGA). 30 figs.

  20. Belt Vision Inspection System

    Broader source: Energy.gov [DOE]

    Mining operations rely on conveyor belts to move mined material from the working face of the mine to a processing plant. When a conveyor belt breaks or stops for unscheduled maintenance, production...

  1. M.P. BELT DETERIORATION. ACCELERATOR STRUCTURE. BELT CAPABILITY

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    1375 M.P. BELT DETERIORATION. ACCELERATOR STRUCTURE. BELT CAPABILITY M. LETOURNEL Centre de.P. belt deterioration is proposed. It takes into account the strain of discharge to which the belt is submitted following the combination, first of a too high belt charge density in addition to the machine

  2. The Gould Belt

    E-Print Network [OSTI]

    Bobylev, V V

    2015-01-01

    This review is devoted to studies of the Gould belt and the Local system. Since the Gould belt is the giant stellar-gas complex closest to the sun, its stellar component is characterized, along with the stellar associations and diffuse clusters, cold atomic and molecular gas, high-temperature coronal gas, and dust contained in it. Questions relating to the kinematic features of the Gould belt are discussed and the most interesting scenarios for its origin and evolution are examined.

  3. Binaries in the Kuiper Belt

    E-Print Network [OSTI]

    Noll, KS; Grundy, WM; Chiang, EI; Margot, J-L; Kern, SD

    2007-01-01

    The relative sizes of Kuiper Belt binaries. Bull. Amer. As-density for binary Kuiper belt object (26308) 1998 SM 165 .the satellite of Kuiper Belt object 2003 EL 61 . Astrophys.

  4. Setting Confidence Belts

    E-Print Network [OSTI]

    Byron P. Roe; Michael B. Woodroofe

    2000-10-13

    We propose using a Bayes procedure with uniform improper prior to determine credible belts for the mean of a Poisson distribution in the presence of background and for the continuous problem of measuring a non-negative quantity $\\theta$ with a normally distributed measurement error. Within the Bayesian framework, these belts are optimal. The credible limits are then examined from a frequentist point of view and found to have good frequentist and conditional frequentist properties.

  5. Belt conveyor apparatus

    DOE Patents [OSTI]

    Oakley, David J. (Richland, WA); Bogart, Rex L. (Kennewick, WA)

    1987-01-01

    A belt conveyor apparatus according to this invention defines a conveyance path including a first pulley and at least a second pulley. An endless belt member is adapted for continuous travel about the pulleys and comprises a lower portion which engages the pulleys and an integral upper portion adapted to receive objects therein at a first location on said conveyance path and transport the objects to a second location for discharge. The upper belt portion includes an opposed pair of longitudinally disposed crest-like members, biased towards each other in a substantially abutting relationship. The crest-like members define therebetween a continuous, normally biased closed, channel along the upper belt portion. Means are disposed at the first and second locations and operatively associated with the belt member for urging the normally biased together crest-like members apart in order to provide access to the continuous channel whereby objects can be received into, or discharged from the channel. Motors are in communication with the conveyance path for effecting the travel of the endless belt member about the conveyance path. The conveyance path can be configured to include travel through two or more elevations and one or more directional changes in order to convey objects above, below and/or around existing structures.

  6. 2015 EPO No. 14 Belt-Conveyor Scale Systems (Rev 09/14) DRAFT Page 1 of 12

    E-Print Network [OSTI]

    2015 EPO No. 14 Belt-Conveyor Scale Systems (Rev 09/14) DRAFT Page 1 of 12 Examination Procedure Outline for Belt-Conveyor Scale Systems Introduction It is recommended that this outline be followed as minimum criteria for examining belt-conveyor scale systems. This document has been prepared as a guide

  7. Thrust bolting: roof bolt support apparatus

    DOE Patents [OSTI]

    Tadolini, Stephen C. (Lakewood, CO); Dolinar, Dennis R. (Golden, CO)

    1992-01-01

    A method of installing a tensioned roof bolt in a borehole of a rock formation without the aid of a mechanical anchoring device or threaded tensioning threads by applying thrust to the bolt (19) as the bonding material (7') is curing to compress the strata (3) surrounding the borehole (1), and then relieving the thrust when the bonding material (7') has cured.

  8. KUIPER BELT OBJECTS David Jewitt

    E-Print Network [OSTI]

    Jewitt, David C.

    KUIPER BELT OBJECTS David Jewitt Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822 BELT OBJECTS Dec 24 1998 Send Proofs to: David Jewitt Institute for Astronomy, 2680 Woodlawn Drive for Annual Reviews of Earth and Planetary Science. #12; Annual Reviews: Kuiper Belt Page 2 CONTENTS Abstract

  9. Deformation of layered rocks in the ramp regions of thrust faults: a study with rock models 

    E-Print Network [OSTI]

    Chester, Judith Savaso

    1985-01-01

    wall at an S/Lr of 0. 20. " . . . . . . " "" . . -" . 43 17 Diagram showing the thrust belt terminology used to refer to locations and structures in the models. . . . . . 47 18 Deformation maps of configuration A models layered with lead and a... of configuration A. 65 xi LIST OF FIGURES (continued) Figure Page 25 Plot of slip across the lowest lead or mica unit of the veneer at the apex of the anticline above the ramp (location c) versus S/Lr for models of configurations A and B. 67 26 27 Plot...

  10. Replace V-Belts with Notched or Synchronous Belt Drives

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

    A properly designed belt power-transmission system offers high efficiency and low noise, requires no lubrication, and presents low maintenance requirements. However, certain...

  11. 2A New Belt for the Van Allen Belts! Soon after launch, NASA's Van Allen

    E-Print Network [OSTI]

    2A New Belt for the Van Allen Belts! Soon after launch, NASA's Van Allen Probes detected a new Third Belt in the Van Allen Radiation Belts that encircle Earth. Located between the Inner and Outer Belts, which have been known to scientists for decades, the third belt is very temporary. It only

  12. SLH Timing Belt Powertrain

    SciTech Connect (OSTI)

    Schneider, Abe

    2014-04-09

    The main goal of this proposal was to develop and test a novel powertrain solution for the SLH hydroEngine?, a low-cost, efficient low-head hydropower technology. Nearly two-thirds of U.S. renewable electricity is produced by hydropower (EIA 2010). According to the U.S. Department of Energy; this amount could be increased by 50% with small hydropower plants, often using already-existing dams (Hall 2004). There are more than 80,000 existing dams, and of these, less than 4% generate power (Blankinship 2009). In addition, there are over 800 irrigation districts in the U.S., many with multiple, non-power, low-head drops. These existing, non-power dams and irrigation drops could be retrofitted to produce distributed, baseload, renewable energy with appropriate technology. The problem is that most existing dams are low-head, or less than 30 feet in height (Ragon 2009). Only about 2% of the available low-head hydropower resource in the U.S. has been developed, leaving more than 70 GW of annual mean potential low-head capacity untapped (Hall 2004). Natel Energy, Inc. is developing a low-head hydropower turbine that operates efficiently at heads less than 6 meters and is cost-effective for deployment across multiple low-head structures. Because of the unique racetrack-like path taken by the prime-movers in the SLH, a flexible powertrain is required. Historically, the only viable technological solution was roller chain. Despite the having the ability to easily attach blades, roller chain is characterized by significant drawbacks, including high cost, wear, and vibration from chordal action. Advanced carbon-#12;fiber-reinforced timing belts have been recently developed which, coupled with a novel belt attachment system developed by Natel Energy, result in a large reduction in moving parts, reduced mass and cost, and elimination of chordal action for increased fatigue life. The work done in this project affirmatively addressed each of the following 3 major uncertainties concerning a timing-belt based hydroEngine ?powertrain: 1. Can a belt handle the high torques and power loads demanded by the SLH? (Yes.) 2. Can the SLH blades be mounted to belt with a connection that can withstand the loads encountered in operation? (Yes.) 3. Can the belt, with blade attachments, live through the required cyclic loading? (Yes.) The research adds to the general understanding of sustainable small hydropower systems by using innovative system testing to develop and demonstrate performance of a novel powertrain solution, enabling a new type of hydroelectric turbine to be commercially developed. The technical effectiveness of the methods investigated has been shown to be positive through an extensive design and testing process accommodating many constraints and goals, with a major emphasis on high cycle fatigue life. Economic feasibility of the innovations has been demonstrated through many iterations of design for manufacturability and cost reduction. The project is of benefit to the public because it has helped to develop a solution to a major problem -- despite the large available potential for new low-head hydropower, high capital costs and high levelized cost of electricity (LCOE) continue to be major barriers to project development. The hydroEngine? represents a significant innovation, leveraging novel fluid mechanics and mechanical configuration to allow lower-cost turbine manufacture and development of low head hydropower resources.

  13. Drive Alive: Teen Seat Belt Survey Program

    E-Print Network [OSTI]

    2010-01-01

    Traffic Safety Facts – Seat Belt Use in 2009 – OverallTraffic Safety Facts – Seat Belt Use in 2008 – DemographicClick-it-or-Ticket Safety Belt Initiative Telephone Survey.

  14. Impacts of Minnesota's Primary Seat Belt Law

    E-Print Network [OSTI]

    Minnesota, University of

    Impacts of Minnesota's Primary Seat Belt Law Frank Douma Center" Six Policies Strongly Supported By Research · Primary seat belt laws · SobrietyMcal Insights of Portland, Maine #12;Primary Seat Belt Laws "Allowing law

  15. Heavy oil reservoirs in the Tulare Fold Belt, Cymric-McKittrick fields, Kern County, California

    SciTech Connect (OSTI)

    Farley, T. (Chevron U.S.A., Bakersfield, CA (USA))

    1990-05-01

    The Tulare fold belt is a series of asymmetric, generally northeast-verging anticlines and synclines in the Pliocene-Pleistocene Tulare Formation that trend northwestward through the Cymric-McKittrick fields. Anticlines within the deformed belt generally originated as fault propagation folds above decollements, the most important of which is the regional decollement on top of the Amnicola sand, the basal Tulare unit. The Amnicola decollement is the northeast subsurface extension of the McKittrick thrust, a low-angle fault that has displaced the Miocene Antelope shale over the Pliocene San Joaquin Formation and locally over the Tulare Formation. The Amnicola decollement is itself deformed by folding related to a younger, deeper decollement near the base of the San Joaquin Formation that merges westward with the Amnicola decollement and defines a zone of faulting associated with the McKittrick thrust Heavy oil reservoirs in the Tulare Formation are currently undergoing active development by thermal recovery techniques. In general, the geometry of heavy oil reservoirs is determined by location within the Tulare fold belt combined with the position of a subhorizontal fluid level trap that forms the updip limit of fluid-saturated rock Reservoir geometry is complicated by complex local structure, discontinuous stratigraphy, and partial depletion of heavy oil reservoirs by fluid withdrawal due to gravity drainage. Proper resolution of fold geometry, fault geometry, and position of the fluid level trap is crucial to the design and monitoring of thermal recovery projects within the Tulare fold belt.

  16. IR Kuiper Belt Constraints

    E-Print Network [OSTI]

    Teplitz, V L; Anderson, J D; Rosenbaum, D C; Scalise, R J; Wentzler, P; Teplitz, Vigdor L.; Anderson, John D.; Rosenbaum, Doris; Scalise, Randall J.; Wentzler, Paul

    1999-01-01

    We compute the temperature and IR signal of particles of radius $a$ and albedo $\\alpha$ at heliocentric distance $R$, taking into account the emissivity effect, and give an interpolating formula for the result. We compare with analyses of COBE DIRBE data by others (including recent detection of the cosmic IR background) for various values of heliocentric distance, $R$, particle radius, $a$, and particle albedo, $\\alpha$. We then apply these results to a recently-developed picture of the Kuiper belt as a two-sector disk with a nearby, low-density sector (40belt IR spectra for various parameter v...

  17. Structure of the eastern Red Rocks and Wind Ridge thrust faults, Wyoming: how a thrust fault gains displacement along strike 

    E-Print Network [OSTI]

    Huntsman, Brent Stanley

    1983-01-01

    OF FIELD MAPPING Methods . Thrust Faults . The Wind Ridge Thrust Fault System The Red Rocks Thrust Fault System CLAY MODEL STUDIES Purpose and Description Model Results DISCUSSION OF RESULTS Kinematics of the Red Rocks Thrust Fault Termination... . Kinematics of the Southern Wind Ridge Thrust Fault . . . A Conceptual Model of the Red Rocks Thrust Fault Termination Implications of the Red Rocks Fault Termination . . . . . . Page V1 V11 1X X1 X11 7 9 17 18 18 21 24 27 35 35 38 49 49...

  18. Evolution and dynamics of a fold-thrust belt: the Sulaiman Range of Pakistan

    E-Print Network [OSTI]

    Reynolds, Kirsty; Copley, Alex; Hussain, Ekbal

    2015-03-09

    (Treloar & Izatt 1993) and is topped by younger Himalayan molasse. The Sulaiman Range is therefore the uplifted and deformed passive margin sequence of the northwestern edge of the Indian Plate, now accreted to eastern edge of the Afghan Block and being... been significant uplift in the Sulaiman Range— Auden (1974) notes that Jurassic limestones have been uplifted over 6 km above the regional level—it is not clear how much shortening has occurred. Jadoon (1991), Humayon et al. (1991) and Banks & Warburton...

  19. Thermal and Structural Constraints on the Tectonic Evolution of the Idaho-Wyoming-Utah Thrust Belt 

    E-Print Network [OSTI]

    Chapman, Shay Michael

    2013-08-09

    ...................................................................................... 14 4. THERMOCHRONOLOGY AND RECONNAISSANCE GEOCHRONOLOGY ... 16 4.1 Thermochronology Methods ................................................................................. 16 4.2 Reconnaissance Geochronology Methods... ............................................................ 19 4.3 Thermochronology Results ................................................................................... 21 4.4 Reconnaissance Geochronology Results ............................................................... 22 4.5 Thermochronology...

  20. Late Cretaceous extension in the hinterland of the Sevier thrust belt,

    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 on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QAsource History View NewTexas:Montezuma, Arizona: Energy ResourcesProject | Open EnergyFlores,Lasernorthwestern

  1. Other Kuiper Belts

    E-Print Network [OSTI]

    M. Jura

    2003-11-28

    When a main sequence star evolves into a red giant and its Kuiper Belt Object's (KBO's) reach a temperature of about 170 K, the dust released during the rapid ice-sublimation of these cometary bodies may lead to a detectable infrared excess at 25 microns, depending upon the mass of the KBO's. Analysis of IRAS data for 66 first ascent red giants with 200 L(Sun) < L < 300 L(Sun) within 150 pc of the Sun provides an upper limit to the mass in KBO's at 45 AU orbital radius that is usually less than about 0.1 M(Earth). With improved infrared data, we may detect systems of KBO's around first ascent red giants that are analogs to our Solar System's KBO's.

  2. Thrust allocation with power management functionality on dynamically positioned vessels

    E-Print Network [OSTI]

    Johansen, Tor Arne

    Thrust allocation with power management functionality on dynamically positioned vessels Aleksander Veksler,1 Tor Arne Johansen,1 Roger Skjetne2 Abstract--A thrust allocation method with capabilities are fairly straightforward. Index Terms--Thrust Allocation, Surface Vessels, Power Man- agement I

  3. Chaos on the conveyor belt

    E-Print Network [OSTI]

    Bulcsú Sándor; Ferenc Járai-Szabó; Tamás Tél; Zoltán Néda

    2013-04-18

    The dynamics of a spring-block train placed on a moving conveyor belt is investigated both by simple experiments and computer simulations. The first block is connected by spring to an external static point, and due to the dragging effect of the belt the blocks undergo complex stick-slip dynamics. A qualitative agreement with the experimental results can only be achieved by taking into account the spatial inhomogeneity of the friction force on the belt's surface, modeled as noise. As a function of the velocity of the conveyor belt and the noise strength, the system exhibits complex, self-organized critical, sometimes chaotic dynamics and phase transition-like behavior. Noise induced chaos and intermittency is also observed. Simulations suggest that the maximum complexity of the dynamical states is achieved for a relatively small number of blocks, around five.

  4. D. Belt 4:30

    E-Print Network [OSTI]

    chenjk

    2007-08-16

    MA 152 – Online Homework iLrn/ThomsonNOW Course Key Code – for Registration & Getting Started. D. Belt 4:30. Note: This system used to be called iLrn, but ...

  5. Belt conveyors for bulk materials. 6th ed.

    SciTech Connect (OSTI)

    NONE

    2007-07-01

    The 16 chapters are entitled: Belt conveyor general applications economics; Design considerations; Characteristics and conveyability of bulk materials; Capacities, belt widths and speeds; Belt conveyor idlers; Belt tension and power engineering; Belt selection; Pulleys and shafts; Curves; Steep angle conveying; Belt cleaners and accessories; Transfer points; Conveyor motor drives and controls; Operation, maintenance and safety; Belt takeups; and Emerging technologies. 6 apps.

  6. 1. THE RADIATION BELTS The outer zone radiation belts consist of energetic elec-

    E-Print Network [OSTI]

    Elkington, Scot R.

    1. THE RADIATION BELTS The outer zone radiation belts consist of energetic elec- trons trapped in the geomagnetic field. The dynamics of the belts are dictated by the global and local electric and mag- netic, A Review of ULF Interactions with Radiation Belt Electrons Scot R. Elkington Laboratory for Atmospheric

  7. 1 The Main Asteroid Belt Carolyn Crow: NASA's Dawn Mission The Main Asteroid Belt

    E-Print Network [OSTI]

    Waliser, Duane E.

    1 The Main Asteroid Belt Carolyn Crow: NASA's Dawn Mission The Main Asteroid Belt Written to the main asteroid belt to visit two of the largest protoplanets, Vesta and Ceres. Using sunlight, a mere accomplished by a spacecraft before. What compelled astronomers to send Dawn to the asteroid belt and what does

  8. THE KUIPER BELT AND THE PRIMORDIAL EVOLUTION

    E-Print Network [OSTI]

    Brown, Michael E.

    THE KUIPER BELT AND THE PRIMORDIAL EVOLUTION OF THE SOLAR SYSTEM A. MORBIDELLI Observatoire de la C. Morbidelli & Brown Abstract. We discuss the structure of the Kuiper belt as it can be inferred from the #12 inclinations and colors{ which clearly show that the belt has lost its pristine structure of a dynamically cold

  9. Conveyer-Belt Alphabet Erik D. Demaine

    E-Print Network [OSTI]

    Demaine, Erik

    Conveyer-Belt Alphabet Erik D. Demaine Martin L. Demaine Bel´en Palop Mathematics is often pursued, and the mathematics, font design, and puzzles that resulted. Conveyer-Belt Problem Suppose we are given several move), and the band as a conveyer belt or rubber band, modeled as a stretchable closed loop

  10. Conveyer Belt Puzzle Font Erik D. Demaine

    E-Print Network [OSTI]

    Demaine, Erik

    Conveyer Belt Puzzle Font Erik D. Demaine Martin L. Demaine Bel´en Palop (a) Input (b) Goal Figure 1: Conveyer belt open problem. Suppose you have a bunch of circular gears glued to a table (disks in the plane), as in Figure 1a. When can you wrap a conveyer belt (or elastic band) around them so

  11. THE KUIPER BELT: OVERVIEW David Jewitt

    E-Print Network [OSTI]

    Jewitt, David C.

    THE KUIPER BELT: OVERVIEW David Jewitt Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI in November 1998 #12;THE KUIPER BELT: OVERVIEW David Jewitt Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA The study of the Kuiper Belt has emerged as one of the leading subjects

  12. FROM KUIPER BELT OBJECT TO COMETARY NUCLEUS

    E-Print Network [OSTI]

    Jewitt, David C.

    FROM KUIPER BELT OBJECT TO COMETARY NUCLEUS David Jewitt Institute for Astronomy, 2680 Woodlawn body populations are related through a common origin in the Kuiper Belt, notably the Centaurs, the Jupiter Family Comets and certain dead-comets. But does primitive material from the Kuiper Belt survive

  13. The Kuiper Belt Harold F. Levison

    E-Print Network [OSTI]

    Levison, Harold F.

    The Kuiper Belt Harold F. Levison Department of Space Sciences Southwest Research Institute Perspective 2. Basic Orbital Dynamics 3. Observations of Kuiper Belt and Related Objects 4. Physical Observations of Trans-Neptunian Objects 5. The Long-Term Stability of Orbits in the Kuiper Belt 6. The Sizes

  14. A BOOSTER SEAT positions the seat belt

    E-Print Network [OSTI]

    A BOOSTER SEAT positions the seat belt so that it fits properly over the stronger parts of your movement during a crash. A SEAT BELT should lie across the upper thighs and be snug across the shoulder; read the vehicle owner's manual on how to install the car seat using the seat belt or LATCH system

  15. Creating Artificial Radiation Belts in the Lab

    E-Print Network [OSTI]

    Mauel, Michael E.

    Creating Artificial Radiation Belts in the Lab or "Some Observations of Hot Plasma Trapped Jeff #12;Outline · The Earth's radiation belts and ring current · Fast-electron interchange instability) fusion. #12;#12;"Artificial Radiation Belts" Van Allen kissing Explorer 4 "good bye" before it's launch

  16. Sun Belt Press Conference September 1, 2015

    E-Print Network [OSTI]

    Hutchens, John

    1 Sun Belt Press Conference September 1, 2015 Remarks by CCU President David A. DeCenzo Good the Sun Belt's invitation to become its 12th member beginning July 1, 2016. We are excited and honored Sun Belt staff as we embark upon this exciting journey. I also want to take this opportunity to thank

  17. THE KUIPER BELT: OVERVIEW David Jewitt

    E-Print Network [OSTI]

    Jewitt, David C.

    THE KUIPER BELT: OVERVIEW David Jewitt Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI in November 1998 #12; THE KUIPER BELT: OVERVIEW David Jewitt Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA The study of the Kuiper Belt has emerged as one of the leading subjects

  18. DYNAMICS OF THE KUIPER BELT RENU MALHOTRA

    E-Print Network [OSTI]

    Levison, Harold F.

    DYNAMICS OF THE KUIPER BELT RENU MALHOTRA Lunar and Planetary Institute MARTIN DUNCAN Queen of the Kuiper Belt is re­ viewed here. Numerical results on long term orbital evolution and dynamical mechanisms underlying the transport of objects out of the Kuiper Belt are discussed. Scenarios about the origin

  19. Simulation Worksheet: Kuiper Belt Interactions Instructor Guidelines

    E-Print Network [OSTI]

    Farritor, Shane

    Simulation Worksheet: Kuiper Belt Interactions Instructor Guidelines The goal of this activity is for students to understand that there are possible orbits in the outer solar system where Kuiper Belt Objects interaction with the asteroid belt and the Kirkwood Gaps. This worksheet makes use of simulations contained

  20. Certification Program SIX SIGMA GREEN BELT

    E-Print Network [OSTI]

    Bandyopadhyay, Antar

    Certification Program for SIX SIGMA GREEN BELT 20th to 24th January 2015 at Kolkata. Copies of certificates for proof of Domicile 5. A participant will be declared as certified Green Belt a Green Belt Certificate. 6. Any candidate failing to qualify the exam will be given another chance

  1. Impacts of Minnesota's Primary Seat Belt Law

    E-Print Network [OSTI]

    Levinson, David M.

    March 2012 Impacts of Minnesota's Primary Seat Belt Law Authors: Frank Douma Nebiyou Tilahun of Minnesota's Primary Seat Belt Law March 2012 6. 7. Author(s) 8. Performing Organization Report No. Frank. Abstract (Limit: 250 words) In the spring of 2009, the Minnesota Legislature changed the state's seat belt

  2. Synchronous and Cogged Fan Belt Performance Assessment

    SciTech Connect (OSTI)

    Cutler, D.; Dean, J.; Acosta, J.

    2014-02-01

    The GSA Regional GPG Team commissioned the National Renewable Energy Laboratory (NREL) to perform monitoring of cogged V-belts and synchronous belts on both a constant volume and a variable air volume fan at the Byron G. Rodgers Federal Building and U.S. Courthouse in Denver, Colorado. These motor/fan combinations were tested with their original, standard V-belts (appropriately tensioned by an operation and maintenance professional) to obtain a baseline for standard operation. They were then switched to the cogged V-belts, and finally to synchronous belts. The power consumption by the motor was normalized for both fan speed and air density changes. This was necessary to ensure that the power readings were not influenced by a change in rotational fan speed or by the power required to push denser air. Finally, energy savings and operation and maintenance savings were compiled into an economic life-cycle cost analysis of the different belt options.

  3. Seat Belt Use Policy Outline the policy regarding use of seat belt in University of Michigan (U-M) vehicles.

    E-Print Network [OSTI]

    Kirschner, Denise

    Seat Belt Use Policy Objective Outline the policy regarding use of seat belt in University belt when operating a U-M vehicle. 2. Operators are also required to ensure that all occupants are adhering to the seat belt use laws when operating a U-M vehicle. 3. State of Michigan seat belt laws

  4. Generating Thrust with a Biologically-Inspired Robotic Ribbon Fin

    E-Print Network [OSTI]

    MacIver, Malcolm A.

    Generating Thrust with a Biologically-Inspired Robotic Ribbon Fin Michael Epstein Mechanical Mechanical Engineering Northwestern University Evanston, Illinois, USA colgate@northwestern.edu Malcolm A. MacIver Mechanical Engineering Biomedical Engineering Northwestern University Evanston, Illinois, USA

  5. Thrust Network Analysis : exploring three-dimensional equilibrium

    E-Print Network [OSTI]

    Block, Philippe (Philippe Camille Vincent)

    2009-01-01

    This dissertation presents Thrust Network Analysis, a new methodology for generating compression-only vaulted surfaces and networks. The method finds possible funicular solutions under gravitational loading within a defined ...

  6. Computational analysis of spiral groove thrust bearings and face seals 

    E-Print Network [OSTI]

    Zirkelback, Nicole Lisa

    1997-01-01

    Analyses for incompressible and compressible spiral groove thrust bearings (SGTBS) and face seals (SGFSS) are presented. A successive approximation linearizes the partial differential equation of pressure that arises in the compressible fluid...

  7. Design of high temperature high speed electromagnetic axial thrust bearing 

    E-Print Network [OSTI]

    Mohiuddin, Mohammad Waqar

    2002-01-01

    The National Aeronautics and Space Administration (NASA) is researching the magnetic bearings to use it as a better alternative to conventional bearings. This research was to develop an axial thrust electromagnetic bearing for high performance jet...

  8. Microstructures and Rheology of a Limestone-Shale Thrust Fault 

    E-Print Network [OSTI]

    Wells, Rachel Kristen

    2011-02-22

    AND RHEOLOGY OF A LIMESTONE-SHALE THRUST FAULT A Thesis by RACHEL KRISTEN WELLS 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 December... 2010 Major Subject: Geology MICROSTRUCTURES AND RHEOLOGY OF A LIMESTONE-SHALE THRUST FAULT A Thesis by RACHEL KRISTEN WELLS Submitted to the Office of Graduate Studies of Texas A&M University in partial fulfillment...

  9. Orbits, masses, and evolution of main belt triple (87) Sylvia

    E-Print Network [OSTI]

    Fang, J; Margot, JL; Margot, JL; Rojo, P

    2012-01-01

    D. 2008, Binaries in the Kuiper Belt, ed. Barucci, M. A. ,Brozovic et al. 2009), main belt triples Kleopatra (DescampsMASSES, AND EVOLUTION OF MAIN BELT TRIPLE (87) SYLVIA J ULIA

  10. Orbits, Masses, and Evolution of Main Belt Triple (87) Sylvia

    E-Print Network [OSTI]

    Fang, Julia; Margot, Jean-Luc; Rojo, Patricio

    2012-01-01

    D. 2008, Binaries in the Kuiper Belt, ed. Barucci, M. A. ,Brozovic et al. 2009), main belt triples Kleopatra (DescampsMASSES, AND EVOLUTION OF MAIN BELT TRIPLE (87) SYLVIA J ULIA

  11. Binary Objects in the Kuiper Belt and Outlying Centaurs: Simulations

    E-Print Network [OSTI]

    Binary Objects in the Kuiper Belt and Outlying Centaurs: Simulations Stephan Kolassa kolassa Abstract. Two exchange reaction scenarios to account for the characteristics of Kuiper belt binaries, Websites and Programs . . . . . . . . . . . . . . . . . . . . . . 10 2 Binary Objects in the Kuiper Belt 11

  12. Geomorphology, kinematic history, and earthquake behavior of the active Kuwana wedge thrust anticline, central Japan

    E-Print Network [OSTI]

    Mueller, Karl

    blind thrusts [Philip and Meghraoui, 1983; Rockwell et al., 1984, 1988; Bullard and Lettis, 1993; Molnar

  13. Green, Black, Lean Six Sigma and Master Black Belt Certifications

    E-Print Network [OSTI]

    Grissino-Mayer, Henri D.

    Green, Black, Lean Six Sigma and Master Black Belt Certifications Green BeLt CertifiCation Candidates may choose from three Green Belts offered: 1) Lean (one week of coursework) 2) Lean Six Sigma (two weeks of coursework) 3) Six Sigma (two weeks of coursework) Green Belt certification is a two

  14. BELT CHARGING SYSTEM M. LETOURNEL and J.-C. OBERLIN

    E-Print Network [OSTI]

    Boyer, Edmond

    1383 BELT CHARGING SYSTEM M. LETOURNEL and J.-C. OBERLIN Centre de Recherches Nucléaires courroie et de déterminer également les possibilités. Abstract. 2014 In M.P. accelerators belts have encountered some difficulties mainly about the belt life time. In the belt charging system, parameters

  15. Electric filter with movable belt electrode

    DOE Patents [OSTI]

    Bergman, W.

    1983-09-20

    A method and apparatus for removing airborne contaminants entrained in a gas or airstream includes an electric filter characterized by a movable endless belt electrode, a grounded electrode, and a filter medium sandwiched there between. Inclusion of the movable, endless belt electrode provides the driving force for advancing the filter medium through the filter, and reduces frictional drag on the filter medium, thereby permitting a wide choice of filter medium materials. Additionally, the belt electrode includes a plurality of pleats in order to provide maximum surface area on which to collect airborne contaminants. 4 figs.

  16. Electric filter with movable belt electrode

    DOE Patents [OSTI]

    Bergman, Werner (Pleasanton, CA)

    1983-01-01

    A method and apparatus for removing airborne contaminants entrained in a gas or airstream includes an electric filter characterized by a movable endless belt electrode, a grounded electrode, and a filter medium sandwiched therebetween. Inclusion of the movable, endless belt electrode provides the driving force for advancing the filter medium through the filter, and reduces frictional drag on the filter medium, thereby permitting a wide choice of filter medium materials. Additionally, the belt electrode includes a plurality of pleats in order to provide maximum surface area on which to collect airborne contaminants.

  17. Problems of millipound thrust measurement. The "Hansen Suspension"

    SciTech Connect (OSTI)

    Carta, David G.

    2014-03-31

    Considered in detail are problems which led to the need and use of the 'Hansen Suspension'. Also discussed are problems which are likely to be encountered in any low level thrust measuring system. The methods of calibration and the accuracies involved are given careful attention. With all parameters optimized and calibration techniques perfected, the system was found capable of a resolution of 10 {mu} lbs. A comparison of thrust measurements made by the 'Hansen Suspension' with measurements of a less sophisticated device leads to some surprising results.

  18. Statewide Estimate of 2012 Safety Belt Use in Texas

    E-Print Network [OSTI]

    Statewide Estimate of 2012 Safety Belt Use in Texas All Passenger Vehicles Passenger Cars Pickups Front Seat--Estimated Safety Belt Use 94.04 94.88 91.71 Driver--Estimated Safety Belt Use 94.66 95.56 92.10 Passenger--Estimated Safety Belt Use 91.05 91.74 82.11 #12;2012 Safety Belt Use in 18 Texas Cities #12

  19. The Compositional Structure of the Asteroid Belt

    E-Print Network [OSTI]

    DeMeo, Francesca E; Walsh, Kevin J; Chapman, Clark R; Binzel, Richard P

    2015-01-01

    The past decade has brought major improvements in large-scale asteroid discovery and characterization with over half a million known asteroids and over 100,000 with some measurement of physical characterization. This explosion of data has allowed us to create a new global picture of the Main Asteroid Belt. Put in context with meteorite measurements and dynamical models, a new and more complete picture of Solar System evolution has emerged. The question has changed from "What was the original compositional gradient of the Asteroid Belt?" to "What was the original compositional gradient of small bodies across the entire Solar System?" No longer is the leading theory that two belts of planetesimals are primordial, but instead those belts were formed and sculpted through evolutionary processes after Solar System formation. This article reviews the advancements on the fronts of asteroid compositional characterization, meteorite measurements, and dynamical theories in the context of the heliocentric distribution of...

  20. A study of binary Kuiper Belt objects

    E-Print Network [OSTI]

    Kern, Susan Diane

    2006-01-01

    About 105 bodies larger than 100km in diameter (Jewitt 1998) reside in the Kuiper Belt, beyond the orbit of Neptune. Since 1992 observational surveys have discovered over one thousand of these objects, believed to be fossil ...

  1. The Possible Belts for Extrasolar Planetary Systems

    E-Print Network [OSTI]

    Ing-Guey Jiang; M. Duncan; D. N. C. Lin

    2006-10-30

    More than 100 extrasolar planets have been discovered since 1990s. Different from the solar system, these planets' orbital eccentricities cover a huge range from 0 to 0.7. Incidently, the first Kuiper Belt Object was discovered in 1992. Thus, an interesting and important question will be whether extrasolar planetary systems could have structures like Kuiper Belt or asteroid belt. We investigate the stability of these planetary systems with different orbital eccentricities by the similar procedures in Rabl & Dvorak (1988) and Holman & Wiegert (1999). We claim that most extrasolar planetary systems can have their own belts at the outer regions. However, we find that the orbits with high--eccentricity is very powerful in depletion of these populations.

  2. Congressional panel makes recommendations on belt safety

    SciTech Connect (OSTI)

    Fiscor, S.

    2007-12-15

    The Mine Improvement and New Emergency Response Act of 2006 (MINER Act) called for a Technical Study Panel to present a review and make recommendations on the use of belt air and the composition and fire retardant properties of belt materials in underground coal mining. In October 2007 the Panel released 20 recommendations publicly. These are presented in the article. Many recommendations encouraged the MSHA to enforce existing laws of maintenance and fire protection or example more vigorously. Maybe the biggest change recommended was that the industry should adopt the Belt Evaluation Laboratory Test (BELT) standard proposed in 1992. Another important recommendation was one that would help eliminate hazards associated with point feeding. 1 photo.

  3. Engineering Research, Development and Technology, FY95: Thrust area report

    SciTech Connect (OSTI)

    1996-02-01

    The mission of the Engineering Research, Development, and Technology Program at Lawrence Livermore National Laboratory (LLNL) is to develop the knowledge base, process technologies, specialized equipment, tools and facilities to support current and future LLNL programs. Engineering`s efforts are guided by a strategy that results in dual benefit: first, in support of Department of Energy missions, such as national security through nuclear deterrence; and second, in enhancing the nation`s economic competitiveness through their collaboration with US industry in pursuit of the most cost-effective engineering solutions to LLNL programs. To accomplish this mission, the Engineering Research, Development, and Technology Program has two important goals: (1) identify key technologies relevant to LLNL programs where they can establish unique competencies, and (2) conduct high-quality research and development to enhance their capabilities and establish themselves as the world leaders in these technologies. To focus Engineering`s efforts, technology thrust areas are identified and technical leaders are selected for each area. The thrust areas are comprised of integrated engineering activities, staffed by personnel from the nine electronics and mechanical engineering divisions, and from other LLNL organizations. This annual report, organized by thrust area, describes Engineering`s activities for fiscal year 1995. The report provides timely summaries of objectives methods, and key results from eight thrust areas: computational electronics and electromagnetics; computational mechanics; microtechnology; manufacturing technology; materials science and engineering; power conversion technologies; nondestructive evaluation; and information engineering.

  4. Thrust Area Report, Engineering Research, Development and Technology

    SciTech Connect (OSTI)

    Langland, R. T.

    1997-02-01

    The mission of the Engineering Research, Development, and Technology Program at Lawrence Livermore National Laboratory (LLNL) is to develop the knowledge base, process technologies, specialized equipment, tools and facilities to support current and future LLNL programs. Engineering`s efforts are guided by a strategy that results in dual benefit: first, in support of Department of Energy missions, such as national security through nuclear deterrence; and second, in enhancing the nation`s economic competitiveness through our collaboration with U.S. industry in pursuit of the most cost- effective engineering solutions to LLNL programs. To accomplish this mission, the Engineering Research, Development, and Technology Program has two important goals: (1) identify key technologies relevant to LLNL programs where we can establish unique competencies, and (2) conduct high-quality research and development to enhance our capabilities and establish ourselves as the world leaders in these technologies. To focus Engineering`s efforts technology {ital thrust areas} are identified and technical leaders are selected for each area. The thrust areas are comprised of integrated engineering activities, staffed by personnel from the nine electronics and mechanical engineering divisions, and from other LLNL organizations. This annual report, organized by thrust area, describes Engineering`s activities for fiscal year 1996. The report provides timely summaries of objectives, methods, and key results from eight thrust areas: Computational Electronics and Electromagnetics; Computational Mechanics; Microtechnology; Manufacturing Technology; Materials Science and Engineering; Power Conversion Technologies; Nondestructive Evaluation; and Information Engineering. Readers desiring more information are encouraged to contact the individual thrust area leaders or authors. 198 refs., 206 figs., 16 tabs.

  5. Optimal dimensionless design and analysis of jet ejectors as compressors and thrust augmenters 

    E-Print Network [OSTI]

    Mohan, Ganesh

    2006-08-16

    A jet ejector may be used as a compressor or to enhance thrust of watercraft or aircraft. Optimization of jet ejectors as compressors and thrust augmenters was conducted using the software GAMBIT (Computer Aided Engineering (CAE) tool for geometry...

  6. Stroke Belt Initiative 1National Heart, Lung, and Blood Institute Stroke Belt Initiative

    E-Print Network [OSTI]

    Shen, Jun

    Stroke Belt Initiative 1National Heart, Lung, and Blood Institute Stroke Belt Initiative NATIONAL HEART, LUNG, AND BLOOD INSTITUTE Project Accomplishments and Lessons Learned Overview Cerebrovascular to those living in other regions of the country. The National Heart, Lung, and Blood Institute (NHLBI

  7. IDENTIFYING COLLISIONAL FAMILIES IN THE KUIPER BELT

    SciTech Connect (OSTI)

    Marcus, Robert A.; Ragozzine, Darin; Murray-Clay, Ruth A.; Holman, Matthew J., E-mail: rmarcus@cfa.harvard.edu [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States)

    2011-05-20

    The identification and characterization of numerous collisional families-clusters of bodies with a common collisional origin-in the asteroid belt has added greatly to the understanding of asteroid belt formation and evolution. More recent study has also led to an appreciation of physical processes that had previously been neglected (e.g., the Yarkovsky effect). Collisions have certainly played an important role in the evolution of the Kuiper Belt as well, though only one collisional family has been identified in that region to date, around the dwarf planet Haumea. In this paper, we combine insights into collisional families from numerical simulations with the current observational constraints on the dynamical structure of the Kuiper Belt to investigate the ideal sizes and locations for identifying collisional families. We find that larger progenitors (r {approx} 500 km) result in more easily identifiable families, given the difficulty in identifying fragments of smaller progenitors in magnitude-limited surveys, despite their larger spread and less frequent occurrence. However, even these families do not stand out well from the background. Identifying families as statistical overdensities is much easier than characterizing families by distinguishing individual members from interlopers. Such identification seems promising, provided the background population is well known. In either case, families will also be much easier to study where the background population is small, i.e., at high inclinations. Overall, our results indicate that entirely different techniques for identifying families will be needed for the Kuiper Belt, and we provide some suggestions.

  8. Satellites of the largest Kuiper belt objects

    E-Print Network [OSTI]

    M. E. Brown; M. A. van Dam; A. H. Bouchez; D. Le Mignant; R. D. Campbell; J. C. Y. Chin; A. Conrad; S. K. Hartman; E. M. Johansson; R. E. Lafon; D. L. Rabinowitz; P. J. Stomski, Jr.; D. M. Summers; C. A. Trujillo; P. L. Wizinowich

    2005-10-03

    We have searched the four brightest objects in the Kuiper belt for the presence of satellites using the newly commissioned Keck Observatory Laser Guide Star Adaptive Optics system. Satellites are seen around three of the four objects: Pluto (whose satellite Charon is well-known), 2003 EL61, and 2003 UB313. The object 2005 FY9, the brightest Kuiper belt object after Pluto, does not have a satellite detectable within 0.4 arcseconds with a brightness of more than 0.5% of the primary. The presence of satellites to 3 of the 4 brightest Kuiper belt objects is inconsistent with the fraction of satellites in the Kuiper belt at large at the 99.1% confidence level, suggesting a different formation mechanism for these largest KBO satellites. The satellites of 2003 EL61 and 2003 UB313, with fractional brightnesses of 5% and 2% of their primaries, respectively, are significantly fainter relative to their primaries than other known Kuiper belt object satellites, again pointing to possible differences in their origin.

  9. Kinematic Peculiarities of Gould Belt Stars

    E-Print Network [OSTI]

    Vadim V. Bobylev

    2005-12-22

    We analyzed the space velocities of Gould Belt stars younger than 125 Myr located at heliocentric distances Belt by assuming the existence of a single kinematic center whose direction was found to be the following: $l_\\circ=128^\\circ$ and $R_\\circ=150$ pc. The linear velocities reach their maximum at a distance of $\\approx300$ pc from the center and are -6 km s$^{-1}$ for the rotation (whose direction coincides with the Galactic rotation) and +4 km s$^{-1}$ for the expansion. The stellar rotation model used here is shown to give a more faithful description of the observed velocity field than the linear model based on the Oort constants $A_G$ and $B_G$. We present evidence that the young clusters $\\beta$ Pic, Tuc/HorA, and TWA belong to the Gould Belt structure.

  10. Pulsar radiation belts and transient radio emission

    E-Print Network [OSTI]

    Q. Luo; D. B. Melrose

    2007-04-22

    It is proposed that radiation belts similar to the ones in the planetary magnetosphere can exist for a pulsar with a relatively long period and a strong magnetic field. In the belts located in the closed field line region near the light cylinder relativistic pairs are trapped and maintained at a density substantially higher than the local Goldreich-Julian corotation density. The trapped plasma can be supplied and replenished by either direct injection of relativistic pairs from acceleration of externally-supplied particles in a dormant outer gap or in situ ionization of the accreted neutral material in the trapping region. The radiation belts can be disrupted by waves that are excited in the region as the result of plasma instabilities or emitted from the surface due to starquakes or stellar oscillations. The disruption can cause an intermittent particle precipitation toward the star producing radio bursts. It is suggested that such bursts may be seen as rotating radio transients (RRATs).

  11. International Space Environment Conference 2001 Radiation Belt Science and Technology

    E-Print Network [OSTI]

    Chan, Anthony Arthur

    International Space Environment Conference 2001 Radiation Belt Science and Technology July 23 devoted to advancing our understanding of Earth's space environment and its effects on technology-27, 2001, Queenstown, New Zealand The International Space Environment Conference 2001: Radiation Belt

  12. Stored energy in conveyor belts - managing the risks

    SciTech Connect (OSTI)

    Goldbeck, L.J.

    2006-11-15

    Employees need to know the dangers of working around conveyors. Safety training on belt tension is discussed. 3 figs.

  13. Poludnista Dorsa, Venus: History and context of a deformation belt

    E-Print Network [OSTI]

    Hansen, Vicki

    Poludnista Dorsa, Venus: History and context of a deformation belt D. A. Young and V. L. Hansen is combined with altimetry data test models of deformation belt evolution in Venus's lowlands. Poludnista Dorsa, a complex 2000-km-long deformation belt, is highly segmented and broadly time transgressive. Long

  14. Visible and Infrared Photometry of Fourteen Kuiper Belt Objects

    E-Print Network [OSTI]

    Davies, John Keith

    Visible and Infrared Photometry of Fourteen Kuiper Belt Objects John K. Davies Joint Astronomy\\GammaJ colors of 14 Kuiper Belt objects using new infrared (J) data combined, in most cases, with simultaneous. Kuiper Belt objects exhibit a wide range of V\\GammaJ colors but there is no correlation with heliocentric

  15. Gears and Belt Drives for Non-Uniform Transmission

    E-Print Network [OSTI]

    Nawratil, Georg

    Gears and Belt Drives for Non-Uniform Transmission Hellmuth Stachel Abstract Ordinarily, gears and belt drives are used for uniform transmission of rotations between parallel axes. Here we focus. Concerning belt drives, we study their relation to tooth profiles and focus on `strict' cases which work

  16. Forming the Kuiper Belt by the Outward Transport of Objects

    E-Print Network [OSTI]

    Levison, Harold F.

    Forming the Kuiper Belt by the Outward Transport of Objects During Neptune's Migration Harold F la C^ote d'Azur, Nice, France To appear in Nature #12;Page 2 The `dynamically cold Kuiper belt unless the cold Kuiper belt originally contained tens of Earth-masses of solids. While several mechanisms

  17. Thesis Proposal Electromagnetic Ion Cyclotron (EMIC) Waves for Radiation Belt

    E-Print Network [OSTI]

    de Weck, Olivier L.

    Thesis Proposal Electromagnetic Ion Cyclotron (EMIC) Waves for Radiation Belt Remediation particles of the Van Allen belts coming from cosmic rays, solar storms, high altitude nuclear explosions regions, as well as an obstacle to exploration and development of space technologies. The "Radiation Belt

  18. Setting confidence belts Byron P. Roe and Michael B. Woodroofe

    E-Print Network [OSTI]

    Woodroofe, Michael B.

    Setting confidence belts Byron P. Roe and Michael B. Woodroofe Department of Physics (B credible belts for the mean of a Poisson distribution in the presence of a background the Bayesian framework, these belts are optimal. The credible limits are then examined from a frequentist point

  19. THE KUIPER BELT AND ITS PRIMORDIAL SCULPTING A. MORBIDELLI

    E-Print Network [OSTI]

    Brown, Michael E.

    THE KUIPER BELT AND ITS PRIMORDIAL SCULPTING A. MORBIDELLI Observatoire de la Côte d'Azur, Nice the structure of the Kuiper belt as it can be inferred from the first decade of observations. In particular, we that the belt has lost its pristine structure of a dynamically cold proto- planetary disk. Understanding how

  20. Bulk Acoustic Resonator Based on Piezoelectric ZnO Belts

    E-Print Network [OSTI]

    Wang, Zhong L.

    Bulk Acoustic Resonator Based on Piezoelectric ZnO Belts Brent A. Buchine, William L. Hughes, F, a bulk acoustic resonator based on ZnO belts is demonstrated. This device shows a great deal of promise-like geometry, making them ideal candidates as SMR, FBAR, and beam resonators.13 However, handling belts can

  1. Forming the Kuiper Belt by the Outward Transport of Objects

    E-Print Network [OSTI]

    Levison, Harold F.

    Forming the Kuiper Belt by the Outward Transport of Objects During Neptune's Migration Harold F + Observatoire de la Câ??ote d'Azur, Nice, France To appear in Nature #12; Page 2 The `dynamically cold Kuiper belt unless the cold Kuiper belt originally contained tens of Earth­masses of solids. While several mechanisms

  2. Gears and belt drives for non-uniform transmission

    E-Print Network [OSTI]

    Nawratil, Georg

    Gears and belt drives for non-uniform transmission Hellmuth Stachel stachel of gearing 2. Non-uniform belt drives 3. On the existence of strict non-uniform belt drives EUCOMES08. Finsterwalder's principle of gearing The driving wheel 1 rotates about O1 through 1, the out-put wheel 2 rotates

  3. THE PLANE OF THE KUIPER BELT Michael E. Brown

    E-Print Network [OSTI]

    Brown, Michael E.

    THE PLANE OF THE KUIPER BELT Michael E. Brown Division of Geological and Planetary Sciences of the Kuiper belt. The derived plane has an inclination with respect to the ecliptic of 1 .86 and an ascending node of 81 .6, with a 1 error in pole position of the plane of 0 .37. The plane of the Kuiper belt

  4. The largest Kuiper belt objects Michael E. Brown

    E-Print Network [OSTI]

    Brown, Michael E.

    The largest Kuiper belt objects Michael E. Brown California Institute of Technology ABSTRACT While for the first decade of the study of the Kuiper belt, a gap existed between the sizes of the relatively small and faint Kuiper belt objects (KBOs) that were being studied and the largest known KBO, Pluto, recent years

  5. Statistical Methods for Detecting Stellar Occultations by Kuiper Belt Objects

    E-Print Network [OSTI]

    Rice, John

    Statistical Methods for Detecting Stellar Occultations by Kuiper Belt Objects: the Taiwanese in the Kuiper Belt, by measuring the rate of occultations of stars by these objects, using an array of three of the solar system. This belt is the source of most short­period comets, those with periods of 200 years

  6. Certification Program SIX SIGMA GREEN BELT at Kolkata

    E-Print Network [OSTI]

    Bandyopadhyay, Antar

    Certification Program for SIX SIGMA GREEN BELT at Kolkata 20th to 24th January 2015. A participant will be declared as certified Green Belt only after passing the GB certification test with minimum 70% marks, and a candidate will be issued a Green Belt Certificate. 11. Any candidate failing

  7. Colors of Kuiper Belt objects : the relationship between KBO colors and Kuiper Belt plane inclination

    E-Print Network [OSTI]

    Kane, Julia Frances

    2006-01-01

    A large population of small, icy bodies orbits the sun just beyond Neptune, known as the Kuiper Belt. These objects, thought to be the progenitors of short period comets, could provide a sample of primordial material in ...

  8. Six Sigma Black Belts Fight For Quality

    E-Print Network [OSTI]

    Vardeman, Stephen B.

    Six Sigma Black Belts Fight For Quality Ron Scott Ross Finnestad Rodney Kalsow IE 361 mini-paper 9/22/00 #12;Six Sigma is a breakthrough management strategy that is revolutionizing the world's top corporations. So what is Six Sigma? "It is a business process that allows companies to drastically improve

  9. Leinhardt et al.: Collisions in the Kuiper Belt 195 Physical Effects of Collisions in the Kuiper Belt

    E-Print Network [OSTI]

    Stewart, Sarah T.

    Leinhardt et al.: Collisions in the Kuiper Belt 195 195 Physical Effects of Collisions in the Kuiper Belt Zoë M. Leinhardt and Sarah T. Stewart Harvard University Peter H. Schultz Brown University Collisions are a major modification process over the history of the Kuiper belt. Recent work illuminates

  10. Thrust faulting in Temblor Range, Kern County, California

    SciTech Connect (OSTI)

    Simonson, R.R.

    1991-02-01

    Surface and subsurface studies confirm the presence of overthrusting in the Temblor Range between Gonyer Canyon and Recruit Pass. In the subsurface, three wells have penetrated the Cree fault, the Hudbay Cree' No. 1 (7,300 ft), the Frantzen Oil Company Cree' No. 1 (5,865 ft) and the Arco Cree Fee' 1A well (5,915 ft). Below the fault, 25 to 35{degree} of westerly dips on the west flank of the sub-thrust Phelps anticline are encountered. The McDonald section below the fault is comprised of siliceous fractured shale which contains live oil and gas showings. A drill-stem test of the interval from 8,247 to 8,510 ft in the Frantzen well resulted in a recovery of 1,200 ft clean 34{degree} oil and 40 MCF per day gas. The shut in pressure was 3,430 lb, which is a normal hydrostatic pressure common to the producing structures in the southern San Joaquin Valley. The equivalent of this interval has produced over 7,000 bbl of oil in the Arco Cree' 1A well. The Arco Cree Fee' No. 1A well crossed the axis of the Phelps Anticline as indicated by good dipmeter and bottomed in Lower Zemorrian at 14,512 ft total depth. This well was not drilled deep enough to reach the Point of Rocks Sand and did not test the gas showings in the lower Miocene section. In the Gonyer Canyon area, subsurface evidence indicated conditions are similar to those in the Cree area because a large structure is present below a thrust fault. It is believed that significant accumulations will be found beneath thrust faults in the eastern part of the Temblor Range where conditions are similar to those that were instrumental in forming fields such as the Elk Hills, B. V. Hills, Belgian Anticline and others.

  11. Direct thrust measurements and modelling of a radio-frequency expanding plasma thruster

    SciTech Connect (OSTI)

    Lafleur, T.; Charles, C.; Boswell, R. W. [Space Plasma, Power and Propulsion Group, Research School of Physics and Engineering, The Australian National University, Canberra ACT 0200 (Australia); Takahashi, K. [Space Plasma, Power and Propulsion Group, Research School of Physics and Engineering, The Australian National University, Canberra ACT 0200 (Australia); Department of Electrical Engineering and Computer Science, Iwate University, Morioka 020-8551 (Japan)

    2011-08-15

    It is shown analytically that the thrust from a simple plasma thruster (in the absence of a magnetic field) is given by the maximum upstream electron pressure, even if the plasma diverges downstream. Direct thrust measurements of a thruster are then performed using a pendulum thrust balance and a laser displacement sensor. A maximum thrust of about 2 mN is obtained at 700 W for a thruster length of 17.5 cm and a flow rate of 0.9 mg s{sup -1}, while a larger thrust of 4 mN is obtained at a similar power for a length of 9.5 cm and a flow rate of 1.65 mg s{sup -1}. The measured thrusts are in good agreement with the maximum upstream electron pressure found from measurements of the plasma parameters and in fair agreement with a simple global approach used to model the thruster.

  12. Thrust and efficiency model for electron-driven magnetic nozzles

    SciTech Connect (OSTI)

    Little, Justin M.; Choueiri, Edgar Y. [Electric Propulsion and Plasma Dynamics Laboratory, Princeton University, Princeton, New Jersey 08544 (United States)] [Electric Propulsion and Plasma Dynamics Laboratory, Princeton University, Princeton, New Jersey 08544 (United States)

    2013-10-15

    A performance model is presented for magnetic nozzle plasmas driven by electron thermal expansion to investigate how the thrust coefficient and beam divergence efficiency scale with the incoming plasma flow and magnetic field geometry. Using a transformation from cylindrical to magnetic coordinates, an approximate analytical solution is derived to the axisymmetric two-fluid equations for a collisionless plasma flow along an applied magnetic field. This solution yields an expression for the half-width at half-maximum of the plasma density profile in the far-downstream region, from which simple scaling relations for the thrust coefficient and beam divergence efficiency are derived. It is found that the beam divergence efficiency is most sensitive to the density profile of the flow into the nozzle throat, with the highest efficiencies occurring for plasmas concentrated along the nozzle axis. Increasing the expansion ratio of the magnetic field leads to efficiency improvements that are more pronounced for incoming plasmas that are not concentrated along the axis. This implies that the additional magnet required to increase the expansion ratio may be worth the added complexity for plasma sources that exhibit poor confinement.

  13. The Kuiper Belt and Other Debris Disks

    E-Print Network [OSTI]

    David Jewitt; Amaya Moro-Martín; Pedro Lacerda

    2008-08-24

    We discuss the current knowledge of the Solar system, focusing on bodies in the outer regions, on the information they provide concerning Solar system formation, and on the possible relationships that may exist between our system and the debris disks of other stars. Beyond the domains of the Terrestrial and giant planets, the comets in the Kuiper belt and the Oort cloud preserve some of our most pristine materials. The Kuiper belt, in particular, is a collisional dust source and a scientific bridge to the dusty "debris disks" observed around many nearby main-sequence stars. Study of the Solar system provides a level of detail that we cannot discern in the distant disks while observations of the disks may help to set the Solar system in proper context.

  14. Kuiper Belt evolution due to dynamical friction

    E-Print Network [OSTI]

    A. Del Popolo; E. Spedicato; M. Gambera

    1999-05-04

    In this paper we study the role of dynamical friction on the evolution of a population of large objects ($m>10^{22}$ g) at heliocentric distances $>70$ AU in the Kuiper Belt. We show that the already flat distribution of these objects must flatten further due to non-spherically symmetric distribution of matter in the Kuiper Belt. Moreover the dynamical drag, produced by dynamical friction, causes objects of masses $\\geq 10^{24} g$ to lose angular momentum and to fall through more central regions in a timescale $\\approx 10^9 yr$. This mechanism is able to transport inwards objects of the size of Pluto, supposing it was created beyond 50 AU, according to a Stern & Colwell's (1997b) suggestion.

  15. QUAOAR: A ROCK IN THE KUIPER BELT

    SciTech Connect (OSTI)

    Fraser, Wesley C.; Brown, Michael E. [Division of Geological and Planetary Sciences, California Institute of Technology, MC 150-21. 1200 E. California Blvd. Pasadena, CA 91125 (United States)

    2010-05-10

    Here we report Wide-Field Planetary Camera 2 observations of the Quaoar-Weywot Kuiper Belt binary. From these observations, we find that Weywot is on an elliptical orbit with an eccentricity of 0.14 {+-} 0.04, a period of 12.438 {+-} 0.005 days, and a semimajor axis of 1.45 {+-} 0.08 x 10{sup 4} km. The orbit reveals a surprisingly high-Quaoar-Weywot system mass of (1.6 {+-} 0.3) x 10{sup 21} kg. Using the surface properties of the Uranian and Neptunian satellites as a proxy for Quaoar's surface, we reanalyze the size estimate from Brown and Trujillo. We find, from a mean of available published size estimates, a diameter for Quaoar of 890 {+-} 70 km. We find Quaoar's density to be {rho} = 4.2 {+-} 1.3gcm{sup -3}, possibly the highest density in the Kuiper Belt.

  16. Chaotic Diffusion of Resonant Kuiper Belt Objects

    E-Print Network [OSTI]

    Matthew S. Tiscareno; Renu Malhotra

    2009-07-06

    We carried out extensive numerical orbit integrations to probe the long-term chaotic dynamics of the two strongest mean motion resonances of Neptune in the Kuiper belt, the 3:2 (Plutinos) and 2:1 (Twotinos). Our primary results include a computation of the relative volumes of phase space characterized by large- and small-resonance libration amplitudes, and maps of resonance stability measured by mean chaotic diffusion rate. We find that Neptune's 2:1 resonance has weaker overall long-term stability than the 3:2 -- only ~15% of Twotinos are projected to survive for 4 Gyr, compared to ~27% of Plutinos, based on an extrapolation from our 1-Gyr integrations. We find that Pluto has only a modest effect, causing a ~4% decrease in the Plutino population that survives to 4 Gyr. Given current observational estimates, and assuming an initial distribution of particles proportional to the local phase space volume in the resonance, we conclude that the primordial populations of Plutinos and Twotinos formerly made up more than half the population of the classical and resonant Kuiper Belt. We also conclude that Twotinos were originally nearly as numerous as Plutinos; this is consistent with predictions from early models of smooth giant planet migration and resonance sweeping of the Kuiper Belt, and provides a useful constraint for more detailed models.

  17. STUDY CITIES IN THE TEXAS SAFETY BELT OBSERVATIONAL SURVEY CONDUCTED BY TEXAS TRANSPORTATION INSTITUTE

    E-Print Network [OSTI]

    STUDY CITIES IN THE TEXAS SAFETY BELT OBSERVATIONAL SURVEY CONDUCTED BY TEXAS TRANSPORTATION INSTITUTE #12;2010 SAFETY BELT USE BY CITY #12;2010 Safety Belt Use In the 18 Texas Cities City Total N Observed % Restrained Total Driver N % Belt Use Total Passenger N % Belt Use Abilene Amarillo Austin

  18. Statewide Estimate of 2011 Safety Belt Use in Texas

    E-Print Network [OSTI]

    Statewide Estimate of 2011 Safety Belt Use in Texas All Passenger Vehicles Passenger Cars Pickups Front Seat--Estimated Safety Belt Use Standard Error Lower 95% confidence limit Upper 95% confidence limit 93.68 2.31 89.15 98.21 94.67 2.28 90.20 99.14 90.81 2.33 86.24 95.38 Driver--Estimated Safety Belt

  19. New compounds will help coal operators comply with BELT standards

    SciTech Connect (OSTI)

    NONE

    2009-04-15

    US coal producers will soon have a new set of conveyor belting standards, which are currently proposed as a rulemaking by the Mine Safety and Health Administration (MSHA), to bring higher levels of resistance to propagation of fire by a secondary source. The new test being put into effect is known as a Belt Evaluation Laboratory Test (BELT). The article, submitted by Fenner Dunlop, discusses the company's testing procedures and the development of conveyors to comply with regulations. 2 photos.

  20. Data Archive and Portal Thrust Area Strategy Report

    SciTech Connect (OSTI)

    Sivaraman, Chitra; Stephan, Eric G.; Macduff, Matt C.; Hagler, Clay D.

    2014-09-30

    This report describes the Data Archive and Portal (DAP), a key capability of the U.S. Department of Energy's Atmosphere to Electron (A2e) initiative. The DAP Thrust Area Planning Group was organized to develop a plan for deploying this capability. Primarily, the report focuses on a distributed system--a DOE Wind Cloud--that functions as a repository for all A2e data. The Wind Cloud will be accessible via an open, easy-to-navigate user interface that facilitates community data access, interaction, and collaboration. DAP management will work with the community, industry, and international standards bodies to develop standards for wind data and to capture important characteristics of all data in the Wind Cloud.

  1. Geologic Setting of the Central Alaskan Hot Springs Belt: Implications...

    Open Energy Info (EERE)

    the Central Alaskan Hot Springs Belt: Implications for Geothermal Resource Capacity and Sustainable Energy Production Jump to: navigation, search OpenEI Reference LibraryAdd to...

  2. Magnetic refrigeration apparatus with belt of ferro or paramagnetic material

    DOE Patents [OSTI]

    Barclay, J.A.; Stewart, W.F.; Henke, M.D.; Kalash, K.E.

    1986-04-03

    A magnetic refrigerator operating in the 12 to 77 K range utilizes a belt which carries ferromagnetic or paramagnetic material and which is disposed in a loop which passes through the center of a solenoidal magnet to achieve cooling. The magnetic material carried by the belt, which can be blocks in frames of a linked belt, can be a mixture of substances with different Curie temperatures arranged such that the Curie temperatures progressively increase from one edge of the belt to the other. This magnetic refrigerator can be used to cool and liquefy hydrogen or other fluids.

  3. Magnetic refrigeration apparatus with belt of ferro or paramagnetic material

    DOE Patents [OSTI]

    Barclay, John A. (Madison, WI); Stewart, Walter F. (Marshall, WI); Henke, Michael D. (Los Alamos, NM); Kalash, Kenneth E. (Los Alamos, NM)

    1987-01-01

    A magnetic refrigerator operating in the 12 to 77K range utilizes a belt which carries ferromagnetic or paramagnetic material and which is disposed in a loop which passes through the center of a solenoidal magnet to achieve cooling. The magnetic material carried by the belt, which can be blocks in frames of a linked belt, can be a mixture of substances with different Curie temperatures arranged such that the Curie temperatures progressively increase from one edge of the belt to the other. This magnetic refrigerator can be used to cool and liquefy hydrogen or other fluids.

  4. COLORS OF INNER DISK CLASSICAL KUIPER BELT OBJECTS

    SciTech Connect (OSTI)

    Romanishin, W. [Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019 (United States); Tegler, S. C. [Department of Physics and Astronomy, Northern Arizona University, Flagstaff, AZ 86011 (United States); Consolmagno, G. J., E-mail: wromanishin@ou.ed, E-mail: Stephen.Tegler@nau.ed, E-mail: gjc@specola.v [Vatican Observatory, Specola Vaticana, V-00120 (Vatican City State, Holy See)

    2010-07-15

    We present new optical broadband colors, obtained with the Keck 1 and Vatican Advanced Technology telescopes, for six objects in the inner classical Kuiper Belt. Objects in the inner classical Kuiper Belt are of interest as they may represent the surviving members of the primordial Kuiper Belt that formed interior to the current position of the 3:2 resonance with Neptune, the current position of the plutinos, or, alternatively, they may be objects formed at a different heliocentric distance that were then moved to their present locations. The six new colors, combined with four previously published, show that the ten inner belt objects with known colors form a neutral clump and a reddish clump in B-R color. Nonparametric statistical tests show no significant difference between the B-R color distribution of the inner disk objects compared to the color distributions of Centaurs, plutinos, or scattered disk objects. However, the B-R color distribution of the inner classical Kuiper Belt Objects does differ significantly from the distribution of colors in the cold (low inclination) main classical Kuiper Belt. The cold main classical objects are predominately red, while the inner classical belt objects are a mixture of neutral and red. The color difference may reveal the existence of a gradient in the composition and/or surface processing history in the primordial Kuiper Belt, or indicate that the inner disk objects are not dynamically analogous to the cold main classical belt objects.

  5. Design and Implementation of a Thrust-Vectored Unmanned Tail-Sitter with Reconfigurable Wings

    E-Print Network [OSTI]

    Benmei, Chen

    and expanded polyolefin (EPO) foam, U-Lion is equipped with an array of avionic components which enable stable. The propulsion of U-Lion comes from a self-fabricated contra-rotating motor fixed on a gimbal mechanism which can change the direction of the motor for the required thrust. This thrust-vectored propulsion system

  6. Electric Energy Challenges of the Future Future Grid Thrust Area 1 White Paper

    E-Print Network [OSTI]

    Electric Energy Challenges of the Future Future Grid Thrust Area 1 White Paper Power Systems Engineering Research Center Empowering Minds to Engineer the Future Electric Energy System #12;Thrust Area 1 White Paper Electric Energy Challenges of the Future Project Team Gerald T. Heydt, Kory Hedman Arizona

  7. The formation of the Kuiper belt by the outward transport of

    E-Print Network [OSTI]

    Morbidelli, Alessandro

    .............................................................. The formation of the Kuiper belt ............................................................................................................................................................................. The `dynamically cold Kuiper belt' consists of objects on low- inclination orbits between ,40 and ,50 AU from size unless the cold Kuiper belt originally contained tens of Earth masses of solids. Although several

  8. The albedo, size, and density of binary Kuiper Belt object (47171) 1999 TC36

    E-Print Network [OSTI]

    2006-01-01

    2005. The formation of Kuiper-belt binaries through exchangeand Density of Binary Kuiper Belt Object (47171) 1999 TC 36emission of the binary Kuiper Belt Object (47171) 1999 TC 36

  9. Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope

    E-Print Network [OSTI]

    2007-01-01

    in the scattered Kuiper Belt. Astrophys. J. , 635, L97-L100.al. (2002). The binary Kuiper-belt object 1998 WW31. Nature,2005). The high-albedo Kuiper Belt object (55565) 2002 AW

  10. Euclid Asteroseismology and Kuiper Belt Objects

    E-Print Network [OSTI]

    Gould, A; Stello, D

    2015-01-01

    Euclid, which is primarily a dark-energy/cosmology mission, may have a microlensing component, consisting of perhaps four dedicated one-month campaigns aimed at the Galactic bulge. We show that such a program would yield excellent auxilliary science, including asteroseimology detections for about 100,000 giant stars, and detection of about 1000 Kuiper Belt Objects (KBOs), down to 2--2.5 mag below the observed break in the KBO luminosity function at I ~26. For the 400 KBOs below the break, Euclid will measure accurate orbits, with fractional period errors <~ 2.5%.

  11. SunBelt Biofuels | 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 on Google Bookmark EERE: Alternative Fuels Data Center Home Page| Open Energy Information Serbia-Enhancing CapacityVectren)Model for the EntireOpenSumpter,Energy GroupSunBelt Biofuels

  12. Corn Belt Energy Corporation | 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 on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX E LISTStar EnergyLawler,CoalConcordiaConsumer ConnectionCoral Power LLC Place:PowerBelt

  13. Tolerance of combined salinity and O2 deficiency in Hordeum marinum accessions from the grain-belt of Western Australia

    E-Print Network [OSTI]

    Malik1,2,3, AI; English1,2, JP; Shepherd1,4, KA; Islam2,5, AKMR; Colmer1,2, TD

    2009-01-01

    accessions from the grain-belt of Western Australia forcollected from the grain-belt of Western Australia. Single

  14. Visible and infrared photometry of Kuiper Belt objects: searching for evidence of trends

    E-Print Network [OSTI]

    Sheppard, Scott S.

    Visible and infrared photometry of Kuiper Belt objects: searching for evidence of trends Neil Mc. © 2003 Elsevier Science (USA). All rights reserved. Keywords: Kuiper Belt objects; Photometry; Infrared

  15. Best Practices for Rural Traffic Safety Georgia's Experience in Increasing Rural Safety Belt Use Rates

    E-Print Network [OSTI]

    Minnesota, University of

    Best Practices for Rural Traffic Safety Georgia's Experience in Increasing Rural Safety Belt Use Enforcement Efforts ­ Checkpoints ­ Messages regarding Seat Belts ­ Messages regarding Rural SB Use

  16. Radiation belt electrons respond to multiple solar wind inputs

    E-Print Network [OSTI]

    Radiation belt electrons respond to multiple solar wind inputs E. J. Rigler,1 M. Wiltberger,1 and D is clearly valuable from a practical standpoint, but the latter helps build confidence in any physical on the fractional or percent variance of radiation belt electron flux that can be attributed to each different solar

  17. Young Stellar Objects in the Gould Belt

    E-Print Network [OSTI]

    Dunham, Michael M; Evans, Neal J; Broekhoven-Fiene, Hannah; Cieza, Lucas; Di Francesco, James; Gutermuth, Robert A; Harvey, Paul M; Hatchell, Jennifer; Heiderman, Amanda; Huard, Tracy; Johnstone, Doug; Kirk, Jason M; Matthews, Brenda C; Miller, Jennifer F; Peterson, Dawn E; Young, Kaisa E

    2015-01-01

    We present the full catalog of Young Stellar Objects (YSOs) identified in the 18 molecular clouds surveyed by the Spitzer Space Telescope "cores to disks" (c2d) and "Gould Belt" (GB) Legacy surveys. Using standard techniques developed by the c2d project, we identify 3239 candidate YSOs in the 18 clouds, 2966 of which survive visual inspection and form our final catalog of YSOs in the Gould Belt. We compile extinction corrected SEDs for all 2966 YSOs and calculate and tabulate the infrared spectral index, bolometric luminosity, and bolometric temperature for each object. We find that 326 (11%), 210 (7%), 1248 (42%), and 1182 (40%) are classified as Class 0+I, Flat-spectrum, Class II, and Class III, respectively, and show that the Class III sample suffers from an overall contamination rate by background AGB stars between 25% and 90%. Adopting standard assumptions, we derive durations of 0.40-0.78 Myr for Class 0+I YSOs and 0.26-0.50 Myr for Flat-spectrum YSOs, where the ranges encompass uncertainties in the ado...

  18. The Dynamical Evolution of the Asteroid Belt

    E-Print Network [OSTI]

    Morbidelli, Alessandro; O'Brien, David P; Minton, David A; Bottke, William F

    2015-01-01

    The asteroid belt is the leftover of the original planetesimal population in the inner solar system. However, currently the asteroids have orbits with all possible values of eccentricities and inclinations compatible with long-term dynamical stability, whereas the initial planetesimal orbits should have been quasi-circular and almost co-planar. The total mass in the asteroid population is a small fraction of that existing primordially. Also, asteroids with different chemical/mineralogical properties are not ranked in an orderly manner with mean heliocentric distance as one could expect from the existence of a radial gradient of the temperature in the proto-planetary disk, but they are partially mixed. These properties show that the asteroid belt has been severely sculpted by one or a series of processes during its lifetime. This paper reviews the processes that have been proposed so far, discussing the properties that they explain and the problems that they are confronted with. Emphasis is paid to the interpl...

  19. WATER ICE IN THE KUIPER BELT

    SciTech Connect (OSTI)

    Brown, M. E.; Fraser, W. C. [Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125 (United States); Schaller, E. L., E-mail: mbrown@caltech.edu [NASA Dryden Aircraft Operations Facility, Palmdale, CA 93550 (United States)

    2012-06-15

    We examine a large collection of low-resolution near-infrared spectra of Kuiper Belt objects (KBOs) and centaurs in an attempt to understand the presence of water ice in the Kuiper Belt. We find that water ice on the surface of these objects occurs in three separate manners: (1) Haumea family members uniquely show surfaces of nearly pure water ice, presumably a consequence of the fragmentation of the icy mantle of a larger differentiated proto-Haumea; (2) large objects with absolute magnitudes of H < 3 (and a limited number to H = 4.5) have surface coverings of water ice-perhaps mixed with ammonia-that appears to be related to possibly ancient cryovolcanism on these large objects; and (3) smaller KBOs and centaurs which are neither Haumea family members nor cold-classical KBOs appear to divide into two families (which we refer to as 'neutral' and 'red'), each of which is a mixture of a common nearly neutral component and either a slightly red or very red component that also includes water ice. A model suggesting that the difference between neutral and red objects due to formation in an early compact solar system either inside or outside, respectively, of the {approx}20 AU methanol evaporation line is supported by the observation that methanol is only detected on the reddest objects, which are those which would be expected to have the most of the methanol containing mixture.

  20. Deformation associated with transverse-thrust ramps: a field and experimental study 

    E-Print Network [OSTI]

    McCaskey, Michael Donald

    1982-01-01

    direction. 2. Marias Pass Location Maps. (A) Generalized geologic map showing location of Marias Pass, and the Lewis Thrust, and (B) schematic diagram illustrates ramp geometries for the Lewis Thrust in the Marias Pass region. 3. Geometry of dip ramp... of Marias Pass showing the location of study sites A, 8, C, and the dip-ramp site at Two Medicine Lake . 85 24. Contour map of the Lewis Thrust surface in the Marias Pass area constructed from sur- vey sites (measured in feet above sea level in order...

  1. Introduction Preparation

    E-Print Network [OSTI]

    Introduction Motivation Preparation Notos' Components Results Conclusions and Future Work Building Problem Description and Motivation Preparation Notation, Passive DNS trends and Anchor Classes Notos Reputation Results Conclusions and Future Work Special thanks to: Damballa Passive DNS data, Malware and BL

  2. INCLINATION MIXING IN THE CLASSICAL KUIPER BELT

    SciTech Connect (OSTI)

    Volk, Kathryn; Malhotra, Renu, E-mail: kvolk@lpl.arizona.edu [Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721 (United States)

    2011-07-20

    We investigate the long-term evolution of the inclinations of the known classical and resonant Kuiper Belt objects (KBOs). This is partially motivated by the observed bimodal inclination distribution and by the putative physical differences between the low- and high-inclination populations. We find that some classical KBOs undergo large changes in inclination over gigayear timescales, which means that a current member of the low-inclination population may have been in the high-inclination population in the past, and vice versa. The dynamical mechanisms responsible for the time variability of inclinations are predominantly distant encounters with Neptune and chaotic diffusion near the boundaries of mean motion resonances. We reassess the correlations between inclination and physical properties including inclination time variability. We find that the size-inclination and color-inclination correlations are less statistically significant than previously reported (mostly due to the increased size of the data set since previous works with some contribution from inclination variability). The time variability of inclinations does not change the previous finding that binary classical KBOs have lower inclinations than non-binary objects. Our study of resonant objects in the classical Kuiper Belt region includes objects in the 3:2, 7:4, 2:1, and eight higher-order mean motion resonances. We find that these objects (some of which were previously classified as non-resonant) undergo larger changes in inclination compared to the non-resonant population, indicating that their current inclinations are not generally representative of their original inclinations. They are also less stable on gigayear timescales.

  3. Orbit determination using modern filters/smoothers and continuous thrust modeling

    E-Print Network [OSTI]

    Folcik, Zachary James

    2008-01-01

    The development of electric propulsion technology for spacecraft has led to reduced costs and longer lifespans for certain types of satellites. Because these satellites frequently undergo continuous thrust, predicting their ...

  4. The Warped Plane of the Classical Kuiper Belt

    E-Print Network [OSTI]

    Eugene Chiang; Hyomin Choi

    2008-06-02

    By numerically integrating the orbits of the giant planets and of test particles over a period of four billion years, we follow the evolution of the location of the midplane of the Kuiper belt. The Classical Kuiper belt conforms to a warped sheet that precesses with a 1.9 Myr period. The present-day location of the Kuiper belt plane can be computed using linear secular perturbation theory: the local normal to the plane is given by the theory's forced inclination vector, which is specific to every semimajor axis. The Kuiper belt plane does not coincide with the invariable plane, but deviates from it by up to a few degrees in stable zones. For example, at a semimajor axis of 38 AU, the local Kuiper belt plane has an inclination of 1.9 deg and a longitude of ascending node of 149.9 deg when referred to the mean ecliptic and equinox of J2000. At a semimajor axis of 43 AU, the local plane has an inclination of 1.9 deg and a nodal longitude of 78.3 deg. Only at infinite semimajor axis does the Kuiper belt plane merge with the invariable plane, whose inclination is 1.6 deg and nodal longitude is 107.7 deg. A Kuiper belt object keeps its inclination relative to the Kuiper belt plane nearly constant, even while the latter plane departs from the trajectory predicted by linear theory. The constancy of relative inclination reflects the undamped amplitude of free oscillation. Current observations of Classical Kuiper belt objects are consistent with the plane being warped by the giant planets alone, but the sample size will need to increase by a few times before confirmation exceeds 3-sigma in confidence. In principle, differences between the theoretically expected plane and the observed plane could be used to infer as yet unseen masses orbiting the Sun, but carrying out such a program would be challenging.

  5. Characteristics of displacement transfer zones associated with thrust faults / by Arthur Francis Xavier O'Keefe 

    E-Print Network [OSTI]

    O'Keefe, Arthur Francis Xavier

    1980-01-01

    CHARAC 'ERZSTZCS OF DZSPLACENENT TRANSFER 'ZONES ASSOCIATED WI H THRUST FAULTS A Thesis by ARTHUR FRANCIS XAVIER O&HEEFE Submitted to the Graduate College of Texas AlkM University in partial fulfillment of the requirement for the degree... of NASTER OF SCIENCE August 1990 Idaho or Subrent: Geology CHARACTERISTICS QF DISPLACEMENT TRANSFER ZONES ASSOCIATED NITS THRUST FAULTS A Thesis by ARTHUR FRANCIS XAVIER 0 'KEEFE Approved ss to style and content by: (Co-chairman of' Commi. tee...

  6. From the Kuiper Belt to JupiterFamily Comets: The Spatial Distribution of Ecliptic Comets

    E-Print Network [OSTI]

    Levison, Harold F.

    From the Kuiper Belt to Jupiter­Family Comets: The Spatial Distribution of Ecliptic Comets Harold F particles as they evolve from Neptune­encountering orbits in the Kuiper belt for up to 1 Gyr or until, that originated in the Kuiper belt. This conclusion assumes that the rate of objects leaving the Kuiper belt has

  7. Rayleigh-Taylor instability, lithospheric dynamics, surface topography at convergent mountain belts, and gravity anomalies

    E-Print Network [OSTI]

    Kraus, Mary

    Rayleigh-Taylor instability, lithospheric dynamics, surface topography at convergent mountain belts sign. For the range of wavelengths appropriate for convergent mountain belts (~150­600 km), calculated for wave numbers relevant to mountain belts. For essentially all mountain belts, however, measured free

  8. Master of Science in Engineering and Technology Management Louisiana Tech University Six Sigma Black Belt Certification

    E-Print Network [OSTI]

    Selmic, Sandra

    Black Belt Certification A Louisiana Tech University Six Sigma Black Belt certification can be obtained, STAT 507 Design and Analysis of Experiments, and INEN 557 Six Sigma Black Belt Project with a B the Louisiana Tech University Six Sigma Black Belt certification. INEN 514 is offered in the fall and spring

  9. GREENGATE AND FABREEKA BELT PERFORMANCE IN A 3.5 MV TANDEM

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    1413 GREENGATE AND FABREEKA BELT PERFORMANCE IN A 3.5 MV TANDEM F. CRISTOFORI Istituto di Fisica of belts used in the 3.5 MV Tandem of C.I.S.E. REVUE DE PHYSIQUE APPLIQUÃ?E TOME 12, OCTOBRE 1977, PAGE belts. Unfortunately there is little information regarding the performance of these belts

  10. MODELING THE EFFECTS OF BELT COMPLIANCE, BACKLASH, AND SLIP ON WEB TENSION AND NEW METHODS FOR

    E-Print Network [OSTI]

    Pagilla, Prabhakar R.

    MODELING THE EFFECTS OF BELT COMPLIANCE, BACKLASH, AND SLIP ON WEB TENSION AND NEW METHODSQuest Information and Learning Company. #12;MODELING THE EFFECTS OF BELT COMPLIANCE, BACKLASH, AND SLIP ON WEB and analysis of the belt compliance 13 2.1 Belt-pulley transmission system

  11. The small numbers of large Kuiper Belt objects

    SciTech Connect (OSTI)

    Schwamb, Megan E. [Institute of Astronomy and Astrophysics, Academia Sinica, 11F of Astronomy-Mathematics Building, National Taiwan University. No. 1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan (China); Brown, Michael E.; Fraser, Wesley C., E-mail: mschwamb@asiaa.sinica.edu.tw [Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125 (United States)

    2014-01-01

    We explore the brightness distribution of the largest and brightest (m(R) < 22) Kuiper Belt Objects (KBOs). We construct a luminosity function of the dynamically excited or hot Kuiper Belt (orbits with inclinations >5°) from the very brightest to m(R) = 23. We find for m(R) ? 23, a single slope appears to describe the luminosity function. We estimate that ?12 KBOs brighter than m(R) ? 19.5 are present in the Kuiper Belt today. With nine bodies already discovered this suggests that the inventory of bright KBOs is nearly complete.

  12. Kinematics of the Gould Belt Based on Open Clusters

    E-Print Network [OSTI]

    Vadim V. Bobylev

    2006-10-15

    We have redetermined kinematic parameters of the Gould Belt using currently available data on the motion of nearby young (log t Belt center: Ro=150 pc and lo=128 degrees. The whole structure is shown to move relative to the local standard of rest at a velocity of 10.7+-0.7 km/s in the direction l=274+-4degrees and b=-1+-3 degrees. Using the derived rotation velocity, we have estimated the virial mass of the Gould Belt to be 1.5E6 Solar mass.

  13. Physical effects of collisions in the Kuiper belt

    E-Print Network [OSTI]

    Zoe M. Leinhardt; Sarah T. Stewart; Peter H. Schultz

    2007-05-27

    Collisions are a major modification process over the history of the Kuiper Belt. Recent work illuminates the complex array of possible outcomes of individual collisions onto porous, volatile bodies. The cumulative effects of such collisions on the surface features, composition, and internal structure of Kuiper Belt Objects are not yet known. In this chapter, we present the current state of knowledge of the physics of cratering and disruptive collisions in KBO analog materials. We summarize the evidence for a rich collisional history in the Kuiper Belt and present the range possible physical modifications on individual objects. The question of how well present day bodies represent primordial planetesimals can be addressed through future studies of the coupled physical and collisional evolution of Kuiper Belt Objects.

  14. MAIN-BELT COMET P/2012 T1 (PANSTARRS)

    E-Print Network [OSTI]

    Hsieh, Henry H.

    We present initial results from observations and numerical analyses aimed at characterizing the main-belt comet P/2012 T1 (PANSTARRS). Optical monitoring observations were made between 2012 October and 2013 February using ...

  15. Nanomaterial modifications on conductivity of coal conveyer belt

    SciTech Connect (OSTI)

    Zhang, J.C.; Zhang, Y.G.; Wang, T.T.; Yang, L.F.; Liu, S.M.; Yang, D.H.; Zhang, M.; Gao, X. [Zhongyuan University of Technology, Zhengzhou (China)

    2008-08-15

    By analyzing the macro electrical properties and the microscopic structure from SEM of nanomaterials modified mine transmission belt samples. The influences of the filling process of inorganic nano particle-filled rubber and PVC polymer on the physical properties of coal transmission belt is reviewed, as well as PTC and NTC effect on the stability of the physical properties and stability of materials. Influence of nano-materials and polymer materials for rubber and temperature changes in the plastic filled refining process. Crosslinker and major filler changes in the amount and filled plastic chain time on the conductivity of coal conveyer belt is studied. Influence of cure temperature. Cure time on the mechanical performance is studied. The microscopic mechanism of macro conductivity change of conveyer belt is discussed.

  16. Collisional Velocities and Rates in Resonant Planetesimal Belts

    E-Print Network [OSTI]

    Martina Queck; Alexander V. Krivov; Miodrag Sremcevic; Philippe Thebault

    2007-07-23

    We consider a belt of small bodies around a star, captured in one of the external or 1:1 mean-motion resonances with a massive perturber. The objects in the belt collide with each other. Combining methods of celestial mechanics and statistical physics, we calculate mean collisional velocities and collisional rates, averaged over the belt. The results are compared to collisional velocities and rates in a similar, but non-resonant belt, as predicted by the particle-in-a-box method. It is found that the effect of the resonant lock on the velocities is rather small, while on the rates more substantial. The collisional rates between objects in an external resonance are by about a factor of two higher than those in a similar belt of objects not locked in a resonance. For Trojans under the same conditions, the collisional rates may be enhanced by up to an order of magnitude. Our results imply, in particular, shorter collisional lifetimes of resonant Kuiper belt objects in the solar system and higher efficiency of dust production by resonant planetesimals in debris disks around other stars.

  17. Forming the Cold Classical Kuiper Belt in a light Disk

    E-Print Network [OSTI]

    Shannon, Andrew; Lithwick, Yoram

    2015-01-01

    Large Kuiper Belt Objects are conventionally thought to have formed out of a massive planetesimal belt that is a few thousand times its current mass. Such a picture, however, is incompatible with multiple lines of evidence. Here, we present a new model for the conglomeration of Cold Classical Kuiper belt objects, out of a solid belt only a few times its current mass, or a few percent of the solid density in a Minimum Mass Solar Nebula. This is made possible by depositing most of the primordial mass in grains of size centimetre or smaller. These grains collide frequently and maintain a dynamically cold belt out of which large bodies grow efficiently: an order-unity fraction of the solid mass can be converted into large bodies, in contrast to the ~0.1% efficiency in conventional models. Such a light belt may represent the true outer edge of the Solar system, and it may have effectively halted the outward migration of Neptune. In addition to the high efficiency, our model can also produce a mass spectrum that pe...

  18. Replace V-Belts with Notched or Synchronous Belt Drives | Department of

    Broader source: Energy.gov (indexed) [DOE]

    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 Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergyTher i nAandSummary From: v2.7 Multiple< Back<<Energy Belt drives

  19. Structural Geology of a Central Segment of the Qilian Shan-Nan Shan Thrust Belt: Implications for the Magnitude of Cenozoic Shortening in the Northeastern Tibetan Plateau

    E-Print Network [OSTI]

    Reith, Robin

    2013-01-01

    characterization of the Gangcha complex in the West Qinling terrane, central China: Journal of the Geological

  20. Structural Geology of a Central Segment of the Qilian Shan-Nan Shan Thrust Belt: Implications for the Magnitude of Cenozoic Shortening in the Northeastern Tibetan Plateau

    E-Print Network [OSTI]

    Reith, Robin

    2013-01-01

    Dong from the Institute of Geomechanics, Chinese Academy ofmethods at the Institute of Geomechanics, Chinese Academy of

  1. Structural Geology of a Central Segment of the Qilian Shan-Nan Shan Thrust Belt: Implications for the Magnitude of Cenozoic Shortening in the Northeastern Tibetan Plateau

    E-Print Network [OSTI]

    Reith, Robin

    2013-01-01

    continental deformation: Geology, Burchfiel, B.C. , Zhang,by lower crustal flow: Geology, 28: 703-706. Cowgill, E. ,in north Qilian: Gansu Geology, 20: 40-44 (in Chinese with

  2. How did the foreland react? Yangtze foreland fold-and-thrust belt deformation related to exhumation of the Dabie Shan ultrahigh-

    E-Print Network [OSTI]

    Hacker, Bradley R.

    , Bradley R. Hacker2 , Ines Gaitzsch1 and Shuwen Dong3 1 Institut fuÈr Geologie, Technische Universita.g. Ames et al., 1996; Hacker et al., 1996; Liou et al., 1996). It forms the eastern part of the Qinling al., 1997; Hacker et al., in press) suggest an extrusion model for exhu- mation which has a reverse

  3. Structural Geology of a Central Segment of the Qilian Shan-Nan Shan Thrust Belt: Implications for the Magnitude of Cenozoic Shortening in the Northeastern Tibetan Plateau

    E-Print Network [OSTI]

    Reith, Robin

    2013-01-01

    2011. Detrital zircon geochronology of pre-Tertiary strata2003a. Detrital-zircon geochronology of the northeasternC.Y. , 2007. SHRIMP U-Pb geochronology of the zircons from

  4. Engineering Research and Development and Technology thrust area report FY92

    SciTech Connect (OSTI)

    Langland, R.T.; Minichino, C.

    1993-03-01

    The mission of the Engineering Research, Development, and Technology Program at Lawrence Livermore National Laboratory (LLNL) is to develop the technical staff and the technology needed to support current and future LLNL programs. To accomplish this mission, the Engineering Research, Development, and Technology Program has two important goals: (1) to identify key technologies and (2) to conduct high-quality work to enhance our capabilities in these key technologies. To help focus our efforts, we identify technology thrust areas and select technical leaders for each area. The thrust areas are integrated engineering activities and, rather than being based on individual disciplines, they are staffed by personnel from Electronics Engineering, Mechanical Engineering, and other LLNL organizations, as appropriate. The thrust area leaders are expected to establish strong links to LLNL program leaders and to industry; to use outside and inside experts to review the quality and direction of the work; to use university contacts to supplement and complement their efforts; and to be certain that we are not duplicating the work of others. This annual report, organized by thrust area, describes activities conducted within the Program for the fiscal year 1992. Its intent is to provide timely summaries of objectives, theories, methods, and results. The nine thrust areas for this fiscal year are: Computational Electronics and Electromagnetics; Computational Mechanics; Diagnostics and Microelectronics; Emerging Technologies; Fabrication Technology; Materials Science and Engineering; Microwave and Pulsed Power; Nondestructive Evaluation; and Remote Sensing and Imaging, and Signal Engineering.

  5. Resistive thrust production can be as crucial as added mass mechanisms for inertial undulatory swimmers

    E-Print Network [OSTI]

    Piñeirua, Miguel; Thiria, Benjamin

    2015-01-01

    In this paper, we address a crucial point regarding the description of moderate to high Reynolds numbers aquatic swimmers. For decades, swimming animals have been classified in two different families of propulsive mechanisms based on the Reynolds number: the "resistive" swimmers, using local friction to produce the necessary thrust force for locomotion at low Reynolds number and the "reactive" swimmers, lying in the high Reynolds range, and using added mass acceleration (described by perfect fluid theory). However, inertial swimmers are also systems that dissipate energy, due to their finite size, therefore involving strong resistive contributions, even for high Reynolds numbers. Using a complete model for the hydrodynamic forces, involving both reactive and resistive contributions, we revisit here the physical mechanisms responsible for the thrust production of such swimmers. We show, for instance, that the resistive part of the force balance is as crucial as added mass effects in the modeling of the thrust ...

  6. Angle stations in or for endless conveyor belts

    DOE Patents [OSTI]

    Steel, Alan (Glasgow, GB6)

    1987-04-07

    In an angle station for an endless conveyor belt, there are presented to each incoming run of the belt stationary curved guide members (18, 19) of the shape of a major segment of a right-circular cylinder and having in the part-cylindrical portion (16 or 17) thereof rectangular openings (15) arranged in parallel and helical paths and through which project small freely-rotatable rollers (14), the continuously-changing segments of the curved surfaces of which projecting through said openings (15) are in attitude to change the direction of travel of the belt (13) through 90.degree. during passage of the belt about the part-cylindrical portion (16 or 17) of the guide member (18 or 19). The rectangular openings (15) are arranged with their longer edges lengthwise of the diagonals representing the mean of the helix but with those of a plurality of the rows nearest to each end of the part-cylindrical portion (16 or 17) slightly out of axial symmetry with said diagonals, being slightly inclined in a direction about the intersections (40) of the diagonals of the main portion of the openings, to provide a "toe-in" attitude in relation to the line of run of the endless conveyor belt.

  7. Structure of Possible Long-lived Asteroid Belts

    E-Print Network [OSTI]

    N. W. Evans; S. A. Tabachnik

    2002-04-24

    High resolution simulations are used to map out the detailed structure of two long-lived stable belts of asteroid orbits in the inner Solar system. The Vulcanoid belt extends from 0.09 to 0.20 astronomical units (au), though with a gaps at 0.15 and 0.18 au corresponding to de-stabilising mean motion resonances with Mercury and Venus. As collisional evolution proceeds slower at larger heliocentric distances, kilometre-sized or larger Vulcanoids are most likely to be found in the region between 0.16 and 0.18 au. The optimum location in which to search for Vulcanoids is at geocentric ecliptic longitudes roughly between 9 and 10 degrees. Dynamically speaking, the Earth-Mars belt between 1.08-1.28 au is an extremely stable repository for asteroids on nearly circular orbits. It is interrupted at 1.21 au due to the 3:4 commensurability with the Earth, while secular resonances with Saturn are troublesome beyond 1.17 au. These detailed maps of the fine structure of the belts can be used to plan search methodologies. Strategies for detecting members of the belts are discussed, including the use of infrared wide-field imaging with VISTA, and forthcoming European Space Agency satellite missions like GAIA and BepiColombo.

  8. JOVIAN EARLY BOMBARDMENT: PLANETESIMAL EROSION IN THE INNER ASTEROID BELT

    SciTech Connect (OSTI)

    Turrini, D.; Coradini, A.; Magni, G., E-mail: diego.turrini@ifsi-roma.inaf.it [Istituto di Astrofisica e Planetologia Spaziali, INAF-IAPS, Via Fosso del Cavaliere 100, 00133, Rome (Italy)

    2012-05-01

    The asteroid belt is an open window on the history of the solar system, as it preserves records of both its formation process and its secular evolution. The progenitors of the present-day asteroids formed in the Solar Nebula almost contemporary to the giant planets. The actual process producing the first generation of asteroids is uncertain, strongly depending on the physical characteristics of the Solar Nebula, and the different scenarios produce very diverse initial size-frequency distributions (SFDs). In this work, we investigate the implications of the formation of Jupiter, plausibly the first giant planet to form, on the evolution of the primordial asteroid belt. The formation of Jupiter triggered a short but intense period of primordial bombardment, previously unaccounted for, which caused an early phase of enhanced collisional evolution in the asteroid belt. Our results indicate that this Jovian Early Bombardment caused the erosion or the disruption of bodies smaller than a threshold size, which strongly depends on the SFD of the primordial planetesimals. If the asteroid belt was dominated by planetesimals less than 100 km in diameter, the primordial bombardment would have caused the erosion of bodies smaller than 200 km in diameter. If the asteroid belt was instead dominated by larger planetesimals, the bombardment would have resulted in the destruction of bodies as big as 500 km.

  9. Direct measurement of the impulse in a magnetic thrust chamber system for laser fusion rocket

    SciTech Connect (OSTI)

    Maeno, Akihiro; Yamamoto, Naoji; Nakashima, Hideki [Interdisciplinary Graduate School of Engineering Science, Kyushu University, 6-1 Kasuga-kouen, Kasuga, Fukuoka 816-8580 (Japan); Fujioka, Shinsuke; Johzaki, Tomoyuki [Institute of Laser Engineering, Osaka University, Suita, Osaka 565-087 (Japan); Mori, Yoshitaka [Graduate School for the Creation of New Photonics Industries, Hamamatsu, Shizuoka 431-1202 (Japan); Sunahara, Atsushi [Institute for Laser Technology, Suita, Osaka 565-087 (Japan)

    2011-08-15

    An experiment is conducted to measure an impulse for demonstrating a magnetic thrust chamber system for laser fusion rocket. The impulse is produced by the interaction between plasma and magnetic field. In the experiment, the system consists of plasma and neodymium permanent magnets. The plasma is created by a single-beam laser aiming at a polystyrene spherical target. The impulse is 1.5 to 2.2 {mu}Ns by means of a pendulum thrust stand, when the laser energy is 0.7 J. Without magnetic field, the measured impulse is found to be zero. These results indicate that the system for generating impulse is working.

  10. Early Proterozoic transcontinental orogenic belts in the United States

    SciTech Connect (OSTI)

    Van Schmus, W.R. . Dept. of Geology); Bickford, M.E. . Dept. of Geology); Condie, K.C. . Dept. Geoscience)

    1993-02-01

    It has been recognized for many years that Early Proterozoic orogenic rocks in the western US range from 1.8 to 1.6 Ga, with a general distribution such that 1.8 to 1.7 Ga rocks underlie Colorado, northern Arizona, and northern New Mexico and 1.7 to 1.6 Ga rocks underlie southern Arizona and southern New Mexico. Recent U-Pb geochronologic and Sm-Nd isotopic studies by a variety of research groups have refined crustal history in the western region and have extended knowledge eastward into the buried midcontinent basement. As a result, the authors propose that 1.8 Ga to 1.6 Ga crust of the US by divided into two distinct, but overlapping, orogenic belts: a 1.8 to 1.7 Ga Inner Accretionary Belt and a 1.7 to 1.6 Ga Outer Tectonic Belt. The Inner Accretionary Belt (IAB) comprises rock suites with compositions and isotopic signatures compatible with origin as juvenile crustal terranes formed as oceanic or off-shore and related terranes that were accreted to southern Laurentia between 1.8 and 1.6 Ga. The IAB includes the Yavapai Province of Arizona, Early Proterozoic basement of Colorado and southern Wyoming, and the basement of Nebraska. The Mojave Province of California may be part of this belt, although it also includes components derived from older Proterozoic or Archean crust. Extension of the IAB eastward from Nebraska is uncertain at present, although coeval rocks that may be eastern manifestations of this 1.8 to 1.7 Ga orogenesis occur in Wisconsin (1.76 Ga granite-rhyolite suite), Ontario (Killarney granite), Labrador (Makkovic Province) and southern Greenland (Ketilidian orogen). The Outer Tectonic Belt (OTB) comprises rock suites which have compositions, structures, and isotopic signature compatible with origin in continental margin tectonic settings between 1.7 and 1.6 Ga.

  11. Page 1 of 4 Fig. 1. Wireless system for bladder volume monitoring. The belt is

    E-Print Network [OSTI]

    Chiao, Jung-Chih

    Page 1 of 4 Fig. 1. Wireless system for bladder volume monitoring. The belt is worn at the waist of the patient. In this conceptual drawing, the belt is moved upward in order to show the implant location

  12. Applications of an Electrostatic High-Voltage Tether to Radiation Belt Remediation

    E-Print Network [OSTI]

    Applications of an Electrostatic High-Voltage Tether to Radiation Belt Remediation by Christopher F.1.1 Magnetic Mirrors and the Van Allen Belts........................... 10 1.1.2 The Loss Cone

  13. THE SURFACE COMPOSITION OF LARGE KUIPER BELT OBJECT 2007 OR10

    E-Print Network [OSTI]

    Brown, M. E.

    We present photometry and spectra of the large Kuiper belt object 2007 OR10. The data show significant near-infrared absorption features due to water ice. While most objects in the Kuiper belt with water ice absorption ...

  14. Land regeneration for the 21st Century in the Mersey Belt

    E-Print Network [OSTI]

    Newlands Land regeneration for the 21st Century in the Mersey Belt objectives Newlands (New in the Mersey Belt to support the social and economic regeneration of the area (phase one 2003-2009); improving

  15. Measurements versus Predictions for a Hybrid (Hydrostatic plus Hydrodynamic Thrust Bearing for a Range of Orifice Diameters 

    E-Print Network [OSTI]

    Esser, Paul R.

    2011-08-08

    the static axial load, which is reacted by a second thrust bearing. The rotor is supported radially by two water-lubricated fluid film journal bearings and is attached to a 30,600 rpm motor via a high speed coupling with very low axial stiffness. Thrust...

  16. Detection of methane on Kuiper Belt Object (50000) Quaoar

    E-Print Network [OSTI]

    E. L. Schaller; M. E. Brown

    2007-10-18

    The near-infrared spectrum of (50000) Quaoar obtained at the Keck Observatory shows distinct absorption features of crystalline water ice, solid methane and ethane, and possibly other higher order hydrocarbons. Quaoar is only the fifth Kuiper belt object on which volatile ices have been detected. The small amount of methane on an otherwise water ice dominated surface suggests that Quaoar is a transition object between the dominant volatile-poor small Kuiper belt objects (KBOs) and the few volatile-rich large KBOs such as Pluto and Eris.

  17. Mantle conveyor beneath the Tethyan collisional belt Thorsten W. Becker a,

    E-Print Network [OSTI]

    Becker, Thorsten W.

    into Eurasia, creating the Bitlis­Zagros collisional belt during the spreading of the Red Sea-Gulf of Aden

  18. Dotiki saves money and time with power tool and belt fasteners

    SciTech Connect (OSTI)

    Bargo, K.

    2009-11-15

    The use of a Hilti power tool to improve belt splice installations to minimise downtime is described. 3 photos.

  19. Non-Perturbative Contribution to the Thrust Distribution in e+ e- Annihilation.

    E-Print Network [OSTI]

    Davison, R A; Webber, Bryan R

    The perturbative expansion of the normalised thrust cross section has the general form R(t) = 1 + ?¯sR1(t) + ?¯ 2 sR2(t) + ?¯ 3 sR3(t) + . . . , (6) where R1 (t) is the leading order (LO) coefficient, R2 (t) is the next-to-leading order (NLO) coefficient, R3 (t...

  20. INTRODUCTION With the Jawaharlal Nehru National Solar Mission, there is a thrust

    E-Print Network [OSTI]

    Narayanan, H.

    INTRODUCTION With the Jawaharlal Nehru National Solar Mission, there is a thrust towards Solar Power in India. To facilitate the development of cost effective Solar Power Plants in India, IIT Bombay is setting up a National Solar Thermal Power Testing, Simulation and Research Facility with the financial

  1. Analysis of Oil Lubricated Thrust Collars for Application in Integrally Geared Compressors 

    E-Print Network [OSTI]

    Cable, Travis Alexander

    2015-07-15

    coefficients are determined. In a lubricated thrust collar and bull gear, a hydrodynamic pressure builds in the lower half of the lubricated zone and lubricant cavitation occurs in the upper half. The minimum film thickness and peak pressure in the lubricated...

  2. Optimal Thrust Characteristics of a Synthetic Jet Actuator for Application in Low Speed

    E-Print Network [OSTI]

    Mohseni, Kamran

    - tuators are built and tested. The current actuator design has a mechanical plunger system to generate thrust has a maximum value for formation numbers between 4 and 5.5, which is in agreement with our model). Most ROV's need significant logistic support, such as escort ships, that could limit their availability

  3. PATENTING AND LICENSING The major thrust of the Technology Transfer Office's activity is directed towards

    E-Print Network [OSTI]

    PATENTING AND LICENSING The major thrust of the Technology Transfer Office's activity that he or she may have created an invention, to promptly report it to the Technology Transfer Office. 2. Patentability Determination After the invention is reported to the Technology Transfer Office

  4. CFD Simulation of Dynamic Thrust and Radial Forces on a Vertical Axis Wind Turbine Blade

    E-Print Network [OSTI]

    Tullis, Stephen

    CFD Simulation of Dynamic Thrust and Radial Forces on a Vertical Axis Wind Turbine Blade K. Mc vibration source of a small scale vertical axis wind turbine. The dynamic loading on the blades of the turbine, as they rotate about the central shaft and travel through a range of relative angles of attack

  5. Test-Theory Correlation Study for an Ultra High Temperature Thrust Magnetic Bearing 

    E-Print Network [OSTI]

    Desireddy, Vijesh R.

    2010-01-14

    1000 lb-f of axial thrust load, when rotating at high speed, in a high temperature environment of 1000 0F. This high temperature magnetic bearing system would be used in high performance, high speed and high temperature applications like space vehicles...

  6. FRC Fusion Reactor for Deep Space The Star Thrust Experiment (STX)

    E-Print Network [OSTI]

    Washington at Seattle, University of

    FRC Fusion Reactor for Deep Space Propulsion The Star Thrust Experiment (STX) an experimental=vchar 2/2ttrip vship=vexhaust vchar=2xtrip/ttrip, =vchar 2/2. Fusion is Necessary for Deep Space Travel Propulsion System Exhaust (km/sec) Chemical 5 Electric 30 FRC at RPPL 200 Thermal Fusion 2000 Fusion Proton

  7. AN OVERVIEW OF THE STAR THRUST EXPERIMENT Kenneth Miller, John Slough, and Alan Hoffman

    E-Print Network [OSTI]

    Washington at Seattle, University of

    AN OVERVIEW OF THE STAR THRUST EXPERIMENT Kenneth Miller, John Slough, and Alan Hoffman University-881-7706 Abstract The Field Reversed Configuration, FRC, is a closed field fusion confinement geometry with great. INTRODUCTION It is recognized that nuclear fusion could be an ideal source for space power and propulsion due

  8. FRC Fusion Reactor for Deep Space STXThe Star Thrust Experiment (STX)

    E-Print Network [OSTI]

    Washington at Seattle, University of

    FRC Fusion Reactor for Deep Space Propulsion STXThe Star Thrust Experiment (STX) an experimental=vchar 2/2ttrip vship=vexhaust vchar=2xtrip/ttrip, =vchar 2/2. Fusion is Necessary for Deep Space Travel Propulsion System Exhaust (km/sec) Chemical 5 Electric 30 FRC at RPPL 200 Thermal Fusion 2000 Fusion Proton

  9. Structure of Earth's outer radiation belt inferred from long-term electron flux dynamics

    E-Print Network [OSTI]

    Vassiliadis, Dimitrios

    mapped the radiation-belt structure by quantifying the electron flux variability over the entire radialStructure of Earth's outer radiation belt inferred from long-term electron flux dynamics D September 2003; published 15 October 2003. [1] We map the spatial structure of the electron belts over

  10. Re-examining the main asteroid belt as the primary source of ancient lunar craters

    E-Print Network [OSTI]

    Richardson Jr., James E.

    Re-examining the main asteroid belt as the primary source of ancient lunar craters David A. Minton craters on the ancient lunar highlands were derived from the main asteroid belt in such a way, postulates that a destabilized contiguous inner extension of the main asteroid belt produced a bombardment

  11. Sculpting the Kuiper Belt by a Stellar Encounter: Constraints from the Oort Cloud and Scattered Disk

    E-Print Network [OSTI]

    Levison, Harold F.

    Sculpting the Kuiper Belt by a Stellar Encounter: Constraints from the Oort Cloud and Scattered belt's outer edge (Melita et al: 2002). Thus, we restrict our study to encounters that could have; solar system: general; Oort cloud 1. Introduction Since its discovery in 1992, the Kuiper belt has

  12. High connectivity across the fragmented chemosynthetic ecosystems of the deep Atlantic Equatorial Belt: efficient

    E-Print Network [OSTI]

    Borges, Rita

    Belt: efficient dispersal mechanisms or questionable endemism? SARA TEIXEIRA,* KARINE OLU,* CAROLE Equatorial Belt (AEB). Here, we combined genetic data (COI) from several taxa to assess the possible distributions in overlooked parts of the deep sea. Keywords: Atlantic equatorial belt, chemosynthetic habitats

  13. Forward: Final Version 2007 January 31 Forward to the University of Arizona Kuiper Belt Book

    E-Print Network [OSTI]

    Jewitt, David C.

    Forward: Final Version 2007 January 31 Forward to the University of Arizona Kuiper Belt Book Only belt since 1992. Those of us whose research has "helped the tree grow", a group which includes most a privilege and what a thrill it is to be able to do science this way. The Kuiper belt is amazing in its

  14. Red-belted clearwing Synanthedon myopaeformis Michigan State University's invasive species factsheets

    E-Print Network [OSTI]

    Isaacs, Rufus

    Red-belted clearwing Synanthedon myopaeformis Michigan State University's invasive species State University IPM Program and M. Philip of Michigan Department of Agriculture. The red-belted. Michigan risk maps for exotic plant pests. Other common names small red-belted clearwing, apple clearwing

  15. Discovery of very large amplitude whistler-mode waves in Earth's radiation belts

    E-Print Network [OSTI]

    California at Berkeley, University of

    Discovery of very large amplitude whistler-mode waves in Earth's radiation belts C. Cattell,1 J. R January 2008. [1] During a passage through the Earth's dawn-side outer radiation belt, whistler-mode waves of magnitude larger than previously observed for whistlers in the radiation belt. Although the peak frequency

  16. Optimal Deployment and Efficient Movement of Mobile Sensor Nodes for Long Belt Coverage

    E-Print Network [OSTI]

    Optimal Deployment and Efficient Movement of Mobile Sensor Nodes for Long Belt Coverage Han Xu is a triangle lattice placement. However, what is the optimal placement in a long belt scenario has not been with shifted node strips for complete belt coverage. We prove its optimality in terms of the lowest node

  17. Outer radiation belt boundary location relative to the magnetopause: Implications for magnetopause shadowing

    E-Print Network [OSTI]

    California at Berkeley, University of

    Outer radiation belt boundary location relative to the magnetopause: Implications for magnetopause fluxes of the outer radiation belt often decrease rapidly in response to solar wind disturbances. If the MPS is essential for outer radiation belt electron losses, a close relationship between the outer edge

  18. Large Kuiper Belt Objects: The Mauna Kea 8k CCD Survey

    E-Print Network [OSTI]

    Jewitt, David C.

    Large Kuiper Belt Objects: The Mauna Kea 8k CCD Survey David Jewitt Institute for Astronomy, 2680 1998 January 14 #12; Large Kuiper Belt Objects Page 2 Abstract We describe a large­area ecliptic survey designed to assess the sky­plane surface density of bright Kuiper Belt Objects. We used a 8192 x 8192 pixel

  19. The energization of relativistic electrons in the outer Van Allen radiation belt

    E-Print Network [OSTI]

    Loss, Daniel

    LETTERS The energization of relativistic electrons in the outer Van Allen radiation belt YUE CHEN online: 1 July 2007; doi:10.1038/nphys655 The origin and dynamics of the Van Allen radiation belts is one. These observations represent an important step towards a more complete physical understanding of radiation belt

  20. CONTROL OF A SHAKING BELT CONVEYOR BY A NOVEL APPLICATION OF FLOQUETLYAPUNOV

    E-Print Network [OSTI]

    Spiteri, Raymond J.

    CONTROL OF A SHAKING BELT CONVEYOR BY A NOVEL APPLICATION OF FLOQUET­LYAPUNOV THEORY Raymond J­orientation of workpieces for grasping by a robot is by means of a shaking belt conveyor. Control of small per­ turbations INTRODUCTION A shaking belt conveyor was proposed in [1] to achieve the self­orientation of workpieces in flexi

  1. Geophys. Res. Lett., 17, 3265, 1998. The Global Response of Relativistic Radiation Belt

    E-Print Network [OSTI]

    Reeves, Geoffrey D.

    Geophys. Res. Lett., 17, 3265, 1998. 1 The Global Response of Relativistic Radiation Belt Electrons of the radiation belts at Lª4, however, there was a single enhancement followed by a gradual decay. Radial profiles electron fluxes increased simultaneously at Lª4-6. (2) During the passage of the cloud the radiation belts

  2. The Kuiper Belt As An Evolved Circumstellar David C. Jewitt 1

    E-Print Network [OSTI]

    Jewitt, David C.

    The Kuiper Belt As An Evolved Circumstellar Disk David C. Jewitt 1 Institute for Astronomy­ called Kuiper Belt is a repository of the solar system's most primitive (volatile­rich) matter with orbital semi­ major axes greater than Neptune's 30 AU) have been discovered. Widely known as Kuiper Belt

  3. Submitted to ApJ; preprint: Jan 11, 2011. Inclination Mixing in the Classical Kuiper Belt

    E-Print Network [OSTI]

    Malhotra, Renu

    Submitted to ApJ; preprint: Jan 11, 2011. Inclination Mixing in the Classical Kuiper Belt Kathryn clas- sical and resonant Kuiper belt objects. This is partially motivated by the ob- served bimodal Kuiper belt undergo large changes in inclination (i > 5 ) over gigayear timescales, which means

  4. Radial distributions of equatorial phase space density for outer radiation belt electrons

    E-Print Network [OSTI]

    California at Berkeley, University of

    Radial distributions of equatorial phase space density for outer radiation belt electrons D. L throughout the outer radiation belt using data from the Solid State Telescopes on THEMIS-D. We estimate for the relativistic and non-relativistic populations. Specifically, the PSD distribution of outer belt relativistic

  5. Johnston et al. 1 Preliminary U-Pb Geochronology of the Tugela Terrane, Natal Belt, eastern

    E-Print Network [OSTI]

    Johnston, Stephen T.

    Johnston et al. 1 Preliminary U-Pb Geochronology of the Tugela Terrane, Natal Belt, eastern South of the Mesoproterozoic Natal belt of eastern South Africa. The Tugela terrane consists of a west-plunging structural granitoid suite. Introduction Mesoproterozoic orogenic belts are common to most continental fragments

  6. LANDSLIDE-DRIVEN EROSION AND TOPOGRAPHIC EVOLUTION OF ACTIVE MOUNTAIN BELTS

    E-Print Network [OSTI]

    Weissel, Jeffrey K.

    LANDSLIDE-DRIVEN EROSION AND TOPOGRAPHIC EVOLUTION OF ACTIVE MOUNTAIN BELTS N. HOVIUS* Department a crucial role in the erosion and topographic evolution of active mountain belts. They drive the expansion from active mountain belts. Here, we illustrate these points with observations from the Southern Alps

  7. Incorporating spectral characteristics of Pc5 waves into three-dimensional radiation belt

    E-Print Network [OSTI]

    Elkington, Scot R.

    Incorporating spectral characteristics of Pc5 waves into three-dimensional radiation belt modeling frequency range on radiation belt electrons in a compressed dipole magnetic field is examined-dimensional radiation belt modeling and the diffusion of relativistic electrons, J. Geophys. Res., 110, A03215, doi:10

  8. Comparison of two approaches to automated PI controller tuning for an industrial weigh belt feeder

    E-Print Network [OSTI]

    Collins, Emmanuel

    Comparison of two approaches to automated PI controller tuning for an industrial weigh belt feeder, are applied to an industrial weigh belt feeder that has significant nonlinearities. Both methods do; Weigh belt feeder 1. Introduction Automated controller tuning is of significant in- terest to control

  9. New Directions in Polyvanadate Chemistry:From Cages and Clusters to Baskets, Belts, Bowls, and Barrels

    E-Print Network [OSTI]

    Yaghi, Omar M.

    New Directions in Polyvanadate Chemistry:From Cages and Clusters to Baskets, Belts, Bowls recently ex- panded beyond classical cage/cluster structures to include hitherto unknown basket, belt, bowl 3.14] The belt-shaped [v,0,,]16-anion D is found in 4,['] where it encircles an [*I Prof. W. G

  10. On the Size-Dependence of the Inclination Distribution of the Main Kuiper Belt

    E-Print Network [OSTI]

    Levison, Harold F.

    On the Size-Dependence of the Inclination Distribution of the Main Kuiper Belt Harold F. Levison We present a new analysis of the currently available orbital elements for the known Kuiper belt objects. In the non-resonant, main Kuiper belt we #12;nd a statistically signi#12;cant relationship

  11. High-temperature deformation in the Neoproterozoic transpressional Ribeira belt, southeast Brazil

    E-Print Network [OSTI]

    Bascou, Jérôme

    High-temperature deformation in the Neoproterozoic transpressional Ribeira belt, southeast Brazil; accepted 12 December 2001 Abstract The Neoproterozoic Ribeira belt is subdivided in two domains of anastomosing transcurrent shear zones parallel to the belt. This contrast is interpreted as reflecting

  12. A planetary system as the origin of structure in Fomalhaut's dust belt

    E-Print Network [OSTI]

    Kalas, Paul G.

    A planetary system as the origin of structure in Fomalhaut's dust belt Paul Kalas1 , James R resolution of 0.5 AU. The dust is distributed in a belt 25 AU wide, with a very sharp inner edge at a radial distance of 133 AU, and we measure an offset of 15 AU between the belt's geometric centre and Fomalhaut

  13. Invited Review for Asteroids/Comets/Meteors 1996 The Dynamical Structure of the Kuiper Belt

    E-Print Network [OSTI]

    Levison, Harold F.

    Invited Review for Asteroids/Comets/Meteors 1996 The Dynamical Structure of the Kuiper Belt H 1 , which was the first of over 30 Kuiper Belt objects with radii ¸ 100--200 km that have now been discovered by groundbased observations. When 1992 QB 1 was discovered, the Kuiper Belt was instantly

  14. LONG-TERM DYNAMICS AND THE ORBITAL INCLINATIONS OF THE CLASSICAL KUIPER BELT OBJECTS

    E-Print Network [OSTI]

    Brown, Michael E.

    LONG-TERM DYNAMICS AND THE ORBITAL INCLINATIONS OF THE CLASSICAL KUIPER BELT OBJECTS Marc J in the region of the classical Kuiper belt (41 AU a 47 AU) to explore the role of dynamical instabilities in sculpting the inclination distribution of the classical Kuiper belt objects (KBOs). We find

  15. THE DESIGN OF THE AUTOMATIC CONTROL SYSTEM OF THE GRIPPING-BELT SPEED IN

    E-Print Network [OSTI]

    Boyer, Edmond

    THE DESIGN OF THE AUTOMATIC CONTROL SYSTEM OF THE GRIPPING-BELT SPEED IN LONG-ROOTSTALK TRADITIONAL.R.China, Tel:13836641830, Email:hjxlcj2006@sina.com Abstract This article aims to design a kind of gripping-belt computer as a core combined with fuzzy PID control algorithm. The system can adjust the gripping-belt speed

  16. A FAUNISTIC SURVEY OF NATIVE BEES IN THE MISSISSIPPI BLACK BELT PRAIRIE

    E-Print Network [OSTI]

    Ray, David

    A FAUNISTIC SURVEY OF NATIVE BEES IN THE MISSISSIPPI BLACK BELT PRAIRIE SURVEY OF NATIVE BEES IN THE MISSISSIPPI BLACK BELT PRAIRIE By Beverly A. McGee Smith of Study: A FAUNISTIC SURVEY OF NATIVE BEES IN THE MISSISSIPPI BLACK BELT

  17. SAID/SAPSrelated VLF waves and the outer radiation belt boundary

    E-Print Network [OSTI]

    Santolik, Ondrej

    SAID/SAPSrelated VLF waves and the outer radiation belt boundary Evgeny Mishin,1 Jay Albert,1 for the alteration of the outer radiation belt boundary during (sub)storms. Citation: Mishin, E., J. Albert, and O. Santolik (2011), SAID/SAPSrelated VLF waves and the outer radiation belt boundary, Geophys. Res. Lett., 38

  18. EXPLORATION OF THE KUIPER BELT BY HIGH-PRECISION PHOTOMETRIC STELLAR OCCULTATIONS: FIRST RESULTS

    E-Print Network [OSTI]

    Roques, Françoise

    EXPLORATION OF THE KUIPER BELT BY HIGH-PRECISION PHOTOMETRIC STELLAR OCCULTATIONS: FIRST RESULTS F detected are caused by Kuiper Belt objects beyond 100 AU from the Sun and hence are the farthest known objects in the solar system. These detections show that the Kuiper Belt is much more extended than

  19. Tectonic and petrologic evolution of the Kodiak batholith and the trenchward belt, Kodiak Island, AK: Contact

    E-Print Network [OSTI]

    Wang, Yang

    and the trenchward belt, Kodiak Island, AK: Contact fault juxtaposition? David W. Farris1 Received 4 March 2009; revised 23 December 2010; accepted 9 March 2010; published 20 July 2010. [1] Two forearc magmatic belts exist in Kodiak Island, the granitic Kodiak batholith and the basaltic trenchward belt. Both are part

  20. EVIDENCE FOR A COLOR DEPENDENCE IN THE SIZE DISTRIBUTION OF MAIN-BELT ASTEROIDS Paul Wiegert

    E-Print Network [OSTI]

    Wiegert, Paul

    EVIDENCE FOR A COLOR DEPENDENCE IN THE SIZE DISTRIBUTION OF MAIN-BELT ASTEROIDS Paul Wiegert ($1 km) main-belt asteroids with the 3.6 m Canada-France-Hawaii Telescope. We observed in two filters axis, the difference between the filters in the inner belt is found to be somewhat less pronounced than

  1. The size of the auroral belt during magnetic storms N. Yokoyama1

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    The size of the auroral belt during magnetic storms N. Yokoyama1 , Y. Kamide1 , and H. Miyaoka2 1 and the Dst index, changes in the size of the auroral belt during magnetic storms are studied. It is found that the equatorward boundary of the belt at midnight expands equatorward, reaching its lowest latitude about one hour

  2. Response of highenergy protons of the inner radiation belt to large magnetic storms

    E-Print Network [OSTI]

    California at Berkeley, University of

    Response of highenergy protons of the inner radiation belt to large magnetic storms Hong Zou,1 belt are found during the large storms. Similar loss events were also measured by the HEO3 satellite. The modeling results based on the stormtime geomagnetic field model (TS04c) and the radiation belt model (AP8

  3. Environment and Planning b: Planning and Design Fringe-belt analysis in France

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    Environment and Planning b: Planning and Design Fringe-belt analysis in France : A Conzenian University Estelle.ducom@paris4.sorbonne.fr - 1 - halshs-00203109,version1-9Jan2008 #12;Fringe-belt analysis in France : A Conzenian approach to urban renewal Abstract : This study is based on the fringe-belt model

  4. Toward Application of an Active Fence for Object Detection, Manipulation and Alignment on Conveyer Belt

    E-Print Network [OSTI]

    Belt Andon Salvarinov Shahram Payandeh Experimental Robotics Laboratory (ERL), School of Engineering This paper presents a novel approach for orienting an object on conveyer belt utilizing an Active Fence for each incoming randomly oriented object . Object alignment on conveyor belt by passive fences [2] is one

  5. Evolution of the Namaqua-Natal Belt, southern Africa A geochronological and isotope geochemical review

    E-Print Network [OSTI]

    Patterson, William P.

    Evolution of the Namaqua-Natal Belt, southern Africa ­ A geochronological and isotope geochemical Available online 10 July 2006 Abstract Juvenile crust formation within the Namaqua-Natal Belt occurred of the Mesoproterozoic evolution of the Namaqua-Natal Belt. Graben formation with associated extrusion of lavas

  6. 3MTM Air-MateTM Belt Mounted High Efficiency Powered Air Purifying Respirator (PAPR)

    E-Print Network [OSTI]

    Acton, Scott

    3MTM Air-MateTM Belt Mounted High Efficiency Powered Air Purifying Respirator (PAPR) Welcome and thank you for choosing the 3MTM Air-MateTM Belt Mounted High Efficiency Powered Air Purifying Respirator text #12;Double click picture to start video Click button to view video text #12;3MTM Air-MateTM Belt

  7. PROCESSES OF URBAN CHANGE: PLANNING AND MONITORING STRATEGIES THROUGH THE APPLICATION OF THE FRINGE BELT

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    BELT MODEL TO NANTES AND RENNES (FRANCE). ESTELLE DUCOM Laboratoire RESO UMR CNRS 6590 Université Rennes 2 Haute Bretagne Estelle.ducom@uhb.fr Abstract : This study is based on the fringe belt model (fringe belts). Formerly at the edge of the built-up area, they are now embedded within it

  8. Recent widening of the tropical belt from global tropopause statistics: Sensitivities

    E-Print Network [OSTI]

    Birner, Thomas

    Recent widening of the tropical belt from global tropopause statistics: Sensitivities Thomas Birner 2010. [1] Several recent studies have shown evidence for a widening of the tropical belt over the past of the resulting widening trend of the tropical belt to these thresholds is investigated using four different

  9. THE SECULAR EVOLUTION OF THE PRIMORDIAL KUIPER BELT Joseph M. Hahn1

    E-Print Network [OSTI]

    Hahn, Joseph M.

    THE SECULAR EVOLUTION OF THE PRIMORDIAL KUIPER BELT Joseph M. Hahn1 Lunar and Planetary Institute to compute the secular evolution of a Kuiper Belt having a variety of masses, and it is shown that the early massive belt was very susceptible to the propagation of low-amplitude apsidal and nodal waves launched

  10. SCULPTING THE KUIPER BELT BY A STELLAR ENCOUNTER: CONSTRAINTS FROM THE OORT CLOUD AND SCATTERED DISK

    E-Print Network [OSTI]

    Morbidelli, Alessandro

    SCULPTING THE KUIPER BELT BY A STELLAR ENCOUNTER: CONSTRAINTS FROM THE OORT CLOUD AND SCATTERED et al. as the cause of the Kuiper belt's outer edge. Thus, we restrict our study to encounters system: formation -- solar system: general 1. INTRODUCTION Since its discovery in 1992, the Kuiper belt

  11. Radiation Belt Activity Indices and Solar Proton Event Alarm on the CRATERRE Project Web Site

    E-Print Network [OSTI]

    Radiation Belt Activity Indices and Solar Proton Event Alarm on the CRATERRE Project Web Site D--Two Radiation Belt Activity Indices, based on electron flux measurement >300 keV and >1.6 MeV, and one Solar updated. Index Terms- CRATERRE project, Radiation belts activity, Space environment I. INTRODUCTION

  12. UT College of Natural Sciences Mandatory Safety Belt Usage in College Vehicles

    E-Print Network [OSTI]

    Jefferys, William

    UT College of Natural Sciences Mandatory Safety Belt Usage in College Vehicles To help ensure concerning the use of safety belts will go into effect immediately. These rules supplement and extend those of the State of Texas and the University of Texas. The term "safety belts" refers to both lap and shoulder

  13. Contrasting the efficiency of radiation belt losses caused by ducted and nonducted whistlermode waves

    E-Print Network [OSTI]

    Cummer, Steven A.

    Contrasting the efficiency of radiation belt losses caused by ducted and nonducted whistlermode, nonducted VLF waves are much less effective in driving radiation belt pitch angle scattering. Citation. Parrot, and J.J. Berthelier (2010), Contrasting the efficiency of radiation belt losses caused by ducted

  14. Retention of canopy lichens after partial-cut harvesting in wet-belt interior cedarhemlock forests,

    E-Print Network [OSTI]

    Northern British Columbia, University of

    Retention of canopy lichens after partial-cut harvesting in wet-belt interior cedar­hemlock forests-growth cedar­hemlock forests of the interior wet-belt of British Columbia are rich in abundance and diversity a zone of high precipitation, the so-called interior wet- belt, which favours the development of lush wet

  15. Toward Application of an Active Fence for Object Detection, Manipulation and Alignment on Conveyer Belt

    E-Print Network [OSTI]

    Belt Andon Salvarinov Shahram Payandeh Experimental Robotics Laboratory ERL, School of Engineering This paper presents a novel approach for orienting an object on conveyer belt utilizing an Active Fence for each incoming randomly oriented object . Object alignment on conveyor belt by passive fences 2 is one

  16. THE MURCHISON GREENSTONE BELT, SOUTH AFRICA: ACCRETED1 SLIVERS WITH CONTRASTING METAMORPHIC CONDITIONS2

    E-Print Network [OSTI]

    Boyer, Edmond

    1 THE MURCHISON GREENSTONE BELT, SOUTH AFRICA: ACCRETED1 SLIVERS WITH CONTRASTING METAMORPHIC.09-2.92 Ga Murchison30 Greenstone Belt (MGB), located in South Africa's Kaapvaal Craton, and discusses deformation patterns observed throughout the belt. These patterns are explained by a N-S compressional36

  17. TIME-RESOLVED PHOTOMETRY OF KUIPER BELT OBJECTS: ROTATIONS, SHAPES, AND PHASE FUNCTIONS

    E-Print Network [OSTI]

    Jewitt, David C.

    TIME-RESOLVED PHOTOMETRY OF KUIPER BELT OBJECTS: ROTATIONS, SHAPES, AND PHASE FUNCTIONS Scott S are less spherical than their main-belt asteroid counterparts, indicating a higher specific angular measured phase darkening for seven Kuiper belt objects in the 0 to 2 phase-angle range. Unlike Pluto

  18. Solar, interplanetary, and magnetospheric parameters for the radiation belt energetic electron flux

    E-Print Network [OSTI]

    Vassiliadis, Dimitrios

    Solar, interplanetary, and magnetospheric parameters for the radiation belt energetic electron flux 2005. [1] In developing models of the radiation belt energetic electron flux, it is important identify its peaks in reference to the radial regions P0 (L = 3.1­4.0, inner edge of the outer belt), P1 (4

  19. ENVIRONMENTAL VARIABLES AFFECTING ANT (FORMICIDAE) COMMUNITY COMPOSITION IN MISSISSIPPI'S BLACK BELT

    E-Print Network [OSTI]

    Ray, David

    BELT AND FLATWOODS REGIONS By JoVonn Grady Hill A Thesis Submitted to the Faculty of Mississippi State COMPOSITION IN MISSISSIPPI'S BLACK BELT AND FLATWOODS REGIONS. By JoVonn Grady Hill Approved: Richard L. Brown (FORMICIDAE) COMMUNITY COMPOSITION IN MISSISSIPPI'S BLACK BELT AND FLATWOODS REGIONS Pages in Study: 72

  20. Metallogeny of precious and base metal mineralization in the Murchison Greenstone Belt, South Africa

    E-Print Network [OSTI]

    Boyer, Edmond

    1 Metallogeny of precious and base metal mineralization in the Murchison Greenstone Belt, South The 3.09-2.97 Ga Murchison Greenstone Belt is an important metallotect in the northern Kaapvaal Craton that the major styles of orogenic Au-Sb and the Cu-Zn VMS mineralization in the Murchison Greenstone Belt

  1. Holocene vegetation and fire dynamics in the supra-mediterranean belt of the Nebrodi Mountains

    E-Print Network [OSTI]

    Bern, Universität

    Holocene vegetation and fire dynamics in the supra-mediterranean belt of the Nebrodi Mountains, a small lake in the supra-mediterranean belt in the Nebrodi Mountains of Sicily (Italy). The data suggest from Sicily. In the thermo-mediterranean belt (i.e. broadleaved evergreen wood- lands

  2. Belt-parallel mantle flow beneath a halted continental collision: The Western Alps Guilhem Barruol a,

    E-Print Network [OSTI]

    Demouchy, Sylvie

    Belt-parallel mantle flow beneath a halted continental collision: The Western Alps Guilhem Barruol belts, is a particularly important objective of "mantle tectonics" that may bring a depth extent a coherent picture of upper mantle anisotropy beneath the belt. The large-scale anisotropy pattern

  3. Solar, interplanetary, and magnetospheric parameters for the radiation belt energetic electron flux

    E-Print Network [OSTI]

    California at Berkeley, University of

    Solar, interplanetary, and magnetospheric parameters for the radiation belt energetic electron flux, and A. J. Klimas (2005), Solar, interplanetary, and magnetospheric parameters for the radiation belt 2005. [1] In developing models of the radiation belt energetic electron flux, it is important

  4. Analysis of the rotational properties of Kuiper belt objects

    E-Print Network [OSTI]

    Pedro Lacerda; Jane Luu

    2006-01-12

    We use optical data on 10 Kuiper Belt objects (KBOs) to investigate their rotational properties. Of the 10, three (30%) exhibit light variations with amplitude delta_m >= 0.15 mag, and 1 out of 10 (10%) has delta_m >= 0.40 mag, which is in good agreement with previous surveys. These data, in combination with the existing database, are used to discuss the rotational periods, shapes, and densities of Kuiper Belt objects. We find that, in the sampled size range, Kuiper Belt objects have a higher fraction of low amplitude lightcurves and rotate slower than main belt asteroids. The data also show that the rotational properties and the shapes of KBOs depend on size. If we split the database of KBO rotational properties into two size ranges with diameter larger and smaller than 400 km, we find that: (1) the mean lightcurve amplitudes of the two groups are different with 98.5% confidence, (2) the corresponding power-law shape distributions seem to be different, although the existing data are too sparse to render this difference significant, and (3) the two groups occupy different regions on a spin period vs. lightcurve amplitude diagram. These differences are interpreted in the context of KBO collisional evolution.

  5. On the Dynamics of Resonant Kuiper Belt Objects

    E-Print Network [OSTI]

    Ing-Guey Jiang; Li-Chin Yeh

    2007-01-29

    We propose a new mechanism of drag-induced resonant capture, which can explain the resonant Kuiper Belt Objects in a natural way. A review and comparison with the traditional mechanism of sweeping capture by the migrating Neptune will be given.

  6. A HYPOTHESIS FOR THE COLOR DIVERSITY OF THE KUIPER BELT

    SciTech Connect (OSTI)

    Brown, M. E.; Fraser, W. C. [Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125 (United States); Schaller, E. L., E-mail: mbrown@caltech.edu [NASA Dryden Aircraft Operations Facility, Palmdale, CA 93550 (United States)

    2011-10-01

    We propose a chemical and dynamical process to explain the surface colors of the Kuiper belt. In our hypothesis, the initial bulk compositions of the bodies themselves can be quite diverse-as is seen in comets-but the early surface compositions are set by volatile evaporation after the objects are formed. Strong gradients in surface composition, coupled with UV and particle irradiation, lead to the surface colors that are seen today. The objects formed in the inner part of the primordial belt retain only H{sub 2}O and CO{sub 2} as the major ice species on their surfaces. Irradiation of these species plausibly results in the dark neutrally colored centaurs and Kuiper belt objects (KBOs). Object formed further in the disk retain CH{sub 3}OH, which has been shown to lead to brighter redder surfaces after irradiation, as seen in the brighter redder centaurs and KBOs. Objects formed at the current location of the cold classical Kuiper belt uniquely retain NH{sub 3}, which has been shown to affect irradiation chemistry and could plausibly lead to the unique colors of these objects. We propose observational and experimental tests of this hypothesis.

  7. Pioneer Anomaly and the Kuiper Belt mass distribution

    E-Print Network [OSTI]

    O. Bertolami; P. Vieira

    2006-06-18

    Pioneer 10 and 11 were the first probes sent to study the outer planets of the Solar System and Pioneer 10 was the first spacecraft to leave the Solar System. Besides their already epic journeys, Pioneer 10 and 11 spacecraft were subjected to an unaccounted effect interpreted as a constant acceleration toward the Sun, the so-called Pioneer anomaly. One of the possibilities put forward for explaining the Pioneer anomaly is the gravitational acceleration of the Kuiper Belt. In this work we examine this hypothesis for various models for the Kuiper Belt mass distribution. We find that the gravitational effect due to the Kuiper Belt cannot account for the Pioneer anomaly. Furthermore, we have also studied the hypothesis that drag forces can explain the the Pioneer anomaly; however we conclude that the density required for producing the Pioneer anomaly is many orders of magnitude greater than those of interplanetary and interstellar dust. Our conclusions suggest that only through a mission, the Pioneer anomaly can be confirmed and further investigated. If a mission with these aims is ever sent to space, it turns out, on account of our results, that it will be also a quite interesting probe to study the mass distribution of the Kuiper Belt.

  8. Effective Conveyor Belt Inspection for Improved Mining Productivity

    SciTech Connect (OSTI)

    Chris Fromme

    2006-06-01

    This document details progress on the project entitled ''Effective Conveyor Belt Inspection for Improved Mining Productivity'' during the period from November 15, 2004 to May 14, 2004. Highlights include fabrication of low-cost prototype hardware, acquisition of infrared thermal data, and initial design of a Smart-Camera based system.

  9. Effective Conveyor Belt Inspection for Improved Mining Productivity

    SciTech Connect (OSTI)

    Chris Fromme

    2006-06-01

    This document details progress on the project entitled ''Effective Conveyor Belt Inspection for Improved Mining Productivity'' during the period from November 15, 2004 to May 14, 2004. Highlights include fabrication of an improved LED lightbar, fabrication of a line-scan sensor head for the Smart-Camera based prototype, and development of prototype vulcanized splice detection algorithms.

  10. PRECIPITATION OF RADIATION BELT ELECTRONS BY LIGHTNING-GENERATED

    E-Print Network [OSTI]

    PRECIPITATION OF RADIATION BELT ELECTRONS BY LIGHTNING-GENERATED MAGNETOSPHERICALLY REFLECTING-order model to estimate the L-shell dependence of the precipitation flux of energetic electrons driven by MR L-shell extent) peak in the precipitation signature can result due to the focusing of the whistler

  11. THE COLLISIONAL DIVOT IN THE KUIPER BELT SIZE DISTRIBUTION

    SciTech Connect (OSTI)

    Fraser, Wesley C. [Division of Geological and Planetary Sciences, California Institute of Technology, MC 150-21, 1200 E. California Blvd. Pasadena, CA 91125 (United States)

    2009-11-20

    This paper presents the results of collisional evolution calculations for the Kuiper Belt starting from an initial size distribution similar to that produced by accretion simulations of that region-a steep power-law large object size distribution that breaks to a shallower slope at r approx 1-2 km, with collisional equilibrium achieved for objects r approx< 0.5 km. We find that the break from the steep large object power law causes a divot, or depletion of objects at r approx 10-20 km, which, in turn, greatly reduces the disruption rate of objects with r approx> 25-50 km, preserving the steep power-law behavior for objects at this size. Our calculations demonstrate that the roll-over observed in the Kuiper Belt size distribution is naturally explained as an edge of a divot in the size distribution; the radius at which the size distribution transitions away from the power law, and the shape of the divot from our simulations are consistent with the size of the observed roll-over, and size distribution for smaller bodies. Both the kink radius and the radius of the divot center depend on the strength scaling law in the gravity regime for Kuiper Belt objects. These simulations suggest that the sky density of r approx 1 km objects is approx10{sup 6}-10{sup 7} objects per square degree. A detection of the divot in the size distribution would provide a measure of the strength of large Kuiper Belt objects, and constrain the shape of the size distribution at the end of accretion in the Kuiper Belt.

  12. MAIN-BELT COMET P/2008 R1 (GARRADD)

    SciTech Connect (OSTI)

    Jewitt, David; Yang Bin; Haghighipour, Nader [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States)], E-mail: jewitt@ifa.hawaii.edu, E-mail: yangbin@ifa.hawaii.edu, E-mail: nader@ifa.hawaii.edu

    2009-05-15

    We present a study of the newly discovered main-belt comet P/2008 R1 (Garradd), an object with the dynamical characteristics of an asteroid and the physical characteristics of a comet. Photometry sets a limit to the effective radius of the nucleus at r{sub e} < 0.7 km (red geometric albedo 0.05 assumed). The coma shows a secular fading in our data caused by the escape of dust particles from the near-nucleus environment. The optical reflection spectrum is a nearly neutral continuum devoid of gaseous emission lines, from which we derive a limit to the cyanide (CN) radical production rate of Q {sub CN}< 1.4 x 10{sup 23} s{sup -1} and infer a mass-loss rate <1.5 kg s{sup -1} at the time of our observations. Unlike the first-reported main-belt comets, P/2008 R1 is not dynamically stable. The nearby 8:3 mean-motion resonance with Jupiter induces dynamical instability on timescales 20-30 Myr. Hence, we conclude that P/2008 R1 has recently arrived from a more stable source elsewhere. The high Tisserand parameter of the orbit (in fact, with T{sub J} = 3.216 it is the highest of any comet) points to a source in the asteroid belt itself, instead of in the Kuiper belt (putative source of the Jupiter family comets). We infer that P/2008 R1 is an icy body from the outer asteroid belt in which sublimation has been triggered by rising temperatures resulting from a decreasing perihelion distance.

  13. Electron Acceleration and Loss in the Earth'sElectron Acceleration and Loss in the Earth's Radiation Belts: The Contribution of WaveRadiation Belts: The Contribution of Wave--

    E-Print Network [OSTI]

    Chan, Anthony Arthur

    's Radiation Belts: The Contribution of WaveRadiation Belts: The Contribution of Wave-- particle.Horne@bas.ac.ukR.Horne@bas.ac.uk Tutorial, GEM, Telluride, Colorado, 25 June 2002 Outline ·· RelevanceRelevance ·· Radiation belt variabilityRadiation belt variability ·· Existing theoriesExisting theories ·· Evidence for wave

  14. MICROWAVE EMISSION FROM THE EDGEWORTH-KUIPER BELT AND THE ASTEROID BELT CONSTRAINED FROM THE WILKINSON MICROWAVE ANISOTROPY PROBE

    SciTech Connect (OSTI)

    Ichikawa, Kazuhide; Fukugita, Masataka [Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582 (Japan)

    2011-08-01

    Objects in the Edgeworth-Kuiper Belt and the main asteroid belt should emit microwaves that may give rise to extra anisotropy signals in the multipole of the cosmic microwave background (CMB) experiment. Constraints are derived from the absence of positive detection of such anisotropies for l {approx}< 50, meaning the total mass of Edgeworth-Kuiper Belt objects is smaller than 0.2 M{sub +}. This limit is consistent with the mass extrapolated from the observable population with the size of a {approx}> 15 km, assuming that the small-object population follows the power law in size dN/da {approx} a{sup -q} with the canonical index expected for collisional equilibrium, q {approx_equal} 3.5, with which 23% of the mass is ascribed to objects smaller than are observationally accessible down to grains. A similar argument applied to the main asteroid belt indicates that the grain population should not increase more quickly than q {approx_equal} 3.6 toward smaller radii, if the grain population follows the power law that continues to observed asteroids with larger radii. Both cases are at or only slightly above the limit that can be physically significant, implying the importance of further tightening the CMB anisotropy limit, which may be attained with observation at higher radio frequencies.

  15. On auroral dynamics observed by HF radar: 1. Equatorward edge of the afternoon-evening diuse luminosity belt

    E-Print Network [OSTI]

    Boyer, Edmond

    luminosity belt M. Uspensky1,4 , P. Eglitis1,2 , H. Opgenoorth1,2 , G. Starkov3 , T. Pulkkinen1 , R. Pellinen luminosity belt (SEEL) and the ionospheric footprint of the inner boundary of the electron plasma sheet wave scattering belt and the intense irregular- ity curtains which include the visual auroral belt

  16. Investigation of the axial and radial thrusts in a centrifugal pump 

    E-Print Network [OSTI]

    Park, Chong Hwan

    1984-01-01

    of the Radial Thrusts Determined by the Experiments and the Two Published Theories -- 55 CHAPTER IV CONCLUSIONS AND RECOMMENDATIONS ------- 77 REFFERENCES 81 V1i APPENDIX A APPENDIX B APPENDIX C APPENDIX D APPENDIX E APPENDIX F APPENDIX G VI TA... TABLE OF CONTENTS (Cont'd) Page 84 92 95 102 109 116 123 135 LIST OF TABLES Table 1 Correction Factor ? Determined from the Page Combined Static Calibration Data ------------- 21 Static Calibration Data (Test gl) ------------ 93 Static...

  17. Preparing Your

    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: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass mapSpeedingProgram Guidelines This document w1.½tankSurfaceSciTechenergyand*Prepare

  18. Tectonic mechanisms associated with PT paths of regional metamorphism: alternatives to single-cycle thrusting and heating

    E-Print Network [OSTI]

    Dundas, Robert G.

    that involved thrusting, that buried rocks faster than they can equilibrate with the ambient geothermal gradient, followed by ther- mal relaxation, which reestablished the ambient geo- thermal gradient in underthrust

  19. Gravity interpretation of the northern Overthrust Belt, Idaho and Wyoming 

    E-Print Network [OSTI]

    Silver, Wendy Ilene

    1979-01-01

    GRAVITY INTERPRETATION OF THE NORTHERN OVERTHRUST BELT, IDAHO AND 'vlYOMING A Thesis by IJENDY ILENE SILVER Submitted to the Graduate College of Texas ARM University in partial fulfillment of the requirements for the deoree of MASTER... OF SCIFNCE December 1979 Major Subject: Geology GRAVITY INTERPRETATION OF THE NORTHERN OVERTHRUST lIELT, . IDAHO AND NYOMING A Thesis by NENDY ILEI'lE 5!, LVER Approved as to style and content by: (Chairman of Committee (Hea o epartment (i~1embe...

  20. The Origin and Evolution of the Asteroid Main Belt

    E-Print Network [OSTI]

    Philip R. Bidstrup; Henning Haack; Anja C. Andersen; Rene Michelsen; John Leif Jorgensen

    2005-11-11

    Using a fully autonomous spacecraft - Bering - we propose to detect and study sub-km asteroids from an orbit within the asteroid Main Belt. The main purpose of the proposed Bering mission is to detect a statistically significant sample of an expected population of approximately 10^(10) main belt asteroids in the size range 1 m to 1 km. These asteroids are too faint to be observed using Earth-based telescopes. Sub-km asteroids can be detected from spacecraft at close range but due to the high relative velocities and the long communication times this requires a fully autonomous spacecraft. Using theoretical estimates of the distribution and abundance of sub-km asteroids we find that the Bering mission would detect approximately 6 new sub-km asteroids per day. With an expected lifetime for the mission of a few years we expect to detect and study several thousand sub-km asteroids. Results from the Bering mission would allow us to: 1) Provide further links between groups of meteorites and their parent asteroids. 2) Constrain the cratering rate at planetary surfaces and thus allow significantly improved cratering ages for terrains on Mars and other planets. 3) Constrain processes that transfer small asteroids from orbits in the main belt to the inner Solar System.

  1. Detection of Small Kuiper Belt Objects by Stellar Occultations

    E-Print Network [OSTI]

    R. Stevenson

    2007-12-10

    Knowledge of the Kuiper Belt is currently limited to those objects that can be detected directly. Objects with diameters less than $\\sim$10km reflect too little light to be detected. These smaller bodies could contain most of the mass in the Kuiper Belt while the abundance of these bodies may constrain the distribution of mass. The overall size distribution of bodies within the Kuiper Belt can also be inferred from the relative abundances of sub-km and larger bodies. Stellar occultations are already used to study dark objects in the Solar System, such as asteroids or planetary rings. Occultation by a KBO of a size comparable to, or larger than, that of the Fresnel Scale will result in Fresnel diffraction. Detection of diffraction effects requires fast multiple-star photometry, which will be conducted in July 2007 using the Orthogonal Parallel Transfer Imaging Camera (OPTIC) mounted on the University of Hawaii 2.2m telescope on Mauna Kea. This paper details how knowledge of the mass and structure of the outer Solar System may be obtained through the detection of serendipitous stellar occultations.

  2. Data From HANE-Generated Radiation Belts and the Origin of Diffusion Theory

    SciTech Connect (OSTI)

    Winske, Dan [Los Alamos National Laboratory

    2012-07-16

    In this presentation we briefly review some of the published data regarding the artificial radiation belts produced by the Starfish and R2 high altitude nuclear explosions in 1962. The data showed slow temporal variations of the belts in altitude (L) and pitch angle ({alpha}) that could be modeled as a diffusion process. That early work formed the basis for more complex radiation belt diffusion models that are in use at present.

  3. Gould Belt Kinematics on the Base of the Open Clusters and Ob-Associations

    E-Print Network [OSTI]

    Vadim V. Bobylev; Anisa T. Bajkova

    2006-08-12

    The kinematic parameters of the Gould Belt are redetermined using modern data on the motion of nearby young ($\\log tBelt centre: $l_\\circ=128^\\circ$ and $R_\\circ=150$ pc. It is shown that the whole structure of the Gould Belt is moving relative to the local standard of rest with a velocity of $10.7\\pm0.7$ km s$^{-1}$ in the direction towards $l=274\\pm4^\\circ$, $b=-1\\pm3^\\circ$. Using the rotation velocity, we obtained the virial estimation of the Gould Belt mass as $1.5\\times 10^6 M_\\odot$.

  4. Structure and anisotropy of the Mexico subduction zone based on Rayleigh-wave analysis and implications for the geometry of the Trans-Mexican Volcanic Belt

    E-Print Network [OSTI]

    Stubailo, I; Beghein, C; Davis, PM

    2012-01-01

    across the central Mexican volcanic belt at 100 W: Spatialcentral Trans-Mexican volcanic belt, Chem. Geol. , 244(3–4),Trans-Mexican volcanic belt: Slab detachment in a subduction

  5. UNBIASED INCLINATION DISTRIBUTIONS FOR OBJECTS IN THE KUIPER BELT

    SciTech Connect (OSTI)

    Gulbis, A. A. S. [South African Astronomical Observatory, P.O. Box 9, Observatory, 7935 Cape Town (South Africa); Elliot, J. L.; Adams, E. R. [Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139-4307 (United States); Benecchi, S. D. [Planetary Science Institute, 1700 East Fort Lowell, Suite 106, Tucson, AZ 85719 (United States); Buie, M. W. [Department of Space Studies, Southwest Research Institute, 1050 Walnut Street 400, Boulder, CO 80302 (United States); Trilling, D. E. [Department of Physics and Astronomy, Northern Arizona University, P.O. Box 6010, Flagstaff, AZ 86011 (United States); Wasserman, L. H., E-mail: amanda@saao.ac.z, E-mail: jle@mit.ed, E-mail: era@mit.ed, E-mail: lhw@lowell.ed, E-mail: susank@psi.ed, E-mail: buie@boulder.swri.ed, E-mail: David.Trilling@nau.ed [Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001 (United States)

    2010-08-15

    Using data from the Deep Ecliptic Survey (DES), we investigate the inclination distributions of objects in the Kuiper Belt. We present a derivation for observational bias removal and use this procedure to generate unbiased inclination distributions for Kuiper Belt objects (KBOs) of different DES dynamical classes, with respect to the Kuiper Belt plane. Consistent with previous results, we find that the inclination distribution for all DES KBOs is well fit by the sum of two Gaussians, or a Gaussian plus a generalized Lorentzian, multiplied by sin i. Approximately 80% of KBOs are in the high-inclination grouping. We find that Classical object inclinations are well fit by sin i multiplied by the sum of two Gaussians, with roughly even distribution between Gaussians of widths 2.0{sup +0.6}{sub -0.5}{sup 0} and 8.1{sup +2.6}{sub -2.1}{sup 0}. Objects in different resonances exhibit different inclination distributions. The inclinations of Scattered objects are best matched by sin i multiplied by a single Gaussian that is centered at 19.1{sup +3.9}{sub -3.6}{sup 0} with a width of 6.9{sup +4.1}{sub -2.7}{sup 0}. Centaur inclinations peak just below 20{sup 0}, with one exceptionally high-inclination object near 80{sup 0}. The currently observed inclination distribution of the Centaurs is not dissimilar to that of the Scattered Extended KBOs and Jupiter-family comets, but is significantly different from the Classical and Resonant KBOs. While the sample sizes of some dynamical classes are still small, these results should begin to serve as a critical diagnostic for models of solar system evolution.

  6. Two new basaltic asteroids in the Outer Main Belt?

    E-Print Network [OSTI]

    R. Duffard; F. Roig

    2008-01-14

    The identification of basaltic asteroids in the asteroid Main Belt and the description of their surface mineralogy is necessary to understand the diversity in the collection of basaltic meteorites. Basaltic asteroids can be identified from their visible reflectance spectra and are classified as V-type in the usual taxonomies. In this work, we report visible spectroscopic observations of two candidate V-type asteroids, (7472) Kumakiri and (10537) 1991 RY16, located in the outer Main Belt (a > 2.85 UA). These candidate have been previously identified by Roig and Gil-Hutton (2006, Icarus 183, 411) using the Sloan Digital Sky Survey colors. The spectroscopic observations have been obtained at the Calar Alto Observatory, Spain, during observational runs in November and December 2006. The spectra of these two asteroids show the steep slope shortwards of 0.70 microns and the deep absorption feature longwards of 0.75 microns that are characteristic of V-type asteroids. However, the presence of a shallow but conspicuous absorption band around 0.65 microns opens some questions about the actual mineralogy of these two asteroids. Such band has never been observed before in basaltic asteroids with the intensity we detected it. We discuss the possibility for this shallow absorption feature to be caused by the presence of chromium on the asteroid surface. Our results indicate that, together with (1459) Magnya, asteroids (7472) Kumakiri and (10537) 1991 RY16 may be the only traces of basaltic material found up to now in the outer Main Belt.

  7. Los Alamos provides HOPE for radiation belt storm probes

    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: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home Room NewsInformationJesse BergkampCentermillion to local UnitedtoHOPE for radiation belt storm

  8. US Synthetic Corp (TRL 4 Component)- The Development of Open, Water Lubricated Polycrystalline Diamond Thrust Bearings for use in Marine Hydrokinetic (MHK) Energy Machines

    Broader source: Energy.gov [DOE]

    US Synthetic Corp (TRL 4 Component) - The Development of Open, Water Lubricated Polycrystalline Diamond Thrust Bearings for use in Marine Hydrokinetic (MHK) Energy Machines

  9. First ultraviolet reflectance measurements of several Kuiper Belt objects, Kuiper Belt object satellites, and new ultraviolet measurements of A Centaur

    SciTech Connect (OSTI)

    Stern, S. A.; Schindhelm, E.; Cunningham, N. J.

    2014-05-01

    We observed the 2600-3200 Å (hereafter, mid-UV) reflectance of two Kuiper Belt Objects (KBOs), two KBO satellites, and a Centaur, using the Hubble Space Telescope (HST) Cosmic Origins Spectrograph (COS). Other than measurements of the Pluto system, these constitute the first UV measurements obtained of KBOs, and KBO satellites, and new HST UV measurements of the Centaur 2060 Chiron. We find significant differences among these objects, constrain the sizes and densities of Haumea's satellites, and report the detection of a possible spectral absorption band in Haumea's spectrum near 3050 Å. Comparisons of these objects to previously published UV reflectance measurements of Pluto and Charon are also made here.

  10. Adiabatic effects on radiation belt electrons at low altitude Weichao Tu1,2

    E-Print Network [OSTI]

    Li, Xinlin

    Adiabatic effects on radiation belt electrons at low altitude Weichao Tu1,2 and Xinlin Li1] The stormtime adiabatic effects of radiation belt electrons mirroring at low altitude are not analogous to those of equatorially mirroring electrons. During the main phase of a geomagnetic storm the adiabatic effects

  11. Modeling the radiation belt electrons with radial diffusion driven by the solar wind

    E-Print Network [OSTI]

    Li, Xinlin

    Modeling the radiation belt electrons with radial diffusion driven by the solar wind A. B. Barker1 October 2005. [1] On the basis of the correlation between the solar wind and radiation belt electron fluxes, we develop a model to simulate the MeV electron phase space density variations from L = 3 to L

  12. Master of Science in Engineering and Technology Management Louisiana Tech University Six Sigma Black Belt Certification

    E-Print Network [OSTI]

    Selmic, Sandra

    Master of Science in Engineering and Technology Management Louisiana Tech University Six Sigma Black Belt Certification A Louisiana Tech University Six Sigma Black Belt certification can be obtained by successfully completing INEN 514 Statistical Analysis for Six Sigma, ENGR 566 Six Sigma and Quality Control

  13. Precambrian Research 136 (2005) 2750 The Wadi Mubarak belt, Eastern Desert of Egypt

    E-Print Network [OSTI]

    Fritz, Harald

    2005-01-01

    Precambrian Research 136 (2005) 27­50 The Wadi Mubarak belt, Eastern Desert of Egypt, Graz, Austria b Mansoura University, Faculty of Science, Geology Department, El Mansoura, Egypt c February 2003; accepted 3 September 2004 Abstract The Wadi Mubarak belt in Egypt strikes west­east (and

  14. Are energetic electrons in the solar wind the source of the outer radiation belt?

    E-Print Network [OSTI]

    Li, Xinlin

    . Mewaldt6 Abstract. Using data from WIND, SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer the outer radiation belt electrons. Al- though lower energy electrons in the solar wind could be a seedAre energetic electrons in the solar wind the source of the outer radiation belt? Xinlin Li,1 D. N

  15. Jumping Neptune Can Explain the Kuiper Belt Kernel

    E-Print Network [OSTI]

    Nesvorny, David

    2015-01-01

    The Kuiper belt is a population of icy bodies beyond the orbit of Neptune. A particularly puzzling and up-to-now unexplained feature of the Kuiper belt is the so-called `kernel', a concentration of orbits with semimajor axes a~44 AU, eccentricities e~0.05, and inclinations ibelt kernel can be explained if Neptune's otherwise smooth migration was interrupted by a discontinuous change of Neptune's semimajor axis when Neptune reached ~28 AU. Before the discontinuity happened, planetesimals located at ~40 AU were swept into Neptune's 2:1 resonance, and were carried with the migrating resonance outwards. The 2:1 resonance was at ~44 AU when Neptune reached ~28 AU. If Neptune's semimajor axis changed by fraction of AU at this point, perhaps because Neptune was scattered off of another planet, the 2:1 population would have been released at ~44 AU, and would remain there to this day. We show that the orbital distribution of bodies produced in this model provides a good match to...

  16. Facile synthesis, phase transition, optical switching and oxidation resistance properties of belt-like VO{sub 2}(A) and VO{sub 2}(M) with a rectangular cross section

    SciTech Connect (OSTI)

    Zhang, Yifu; Huang, Yanfen; Zhang, Juecheng; Wu, Weibing; Niu, Fei; Zhong, Yalan [College of Chemistry and Molecular Sciences, Wuhan University, Wuhan 430072 (China)] [College of Chemistry and Molecular Sciences, Wuhan University, Wuhan 430072 (China); Liu, Xinghai, E-mail: liuxh@whu.edu.cn [School of Printing and Packaging, Wuhan University, Wuhan 430079 (China)] [School of Printing and Packaging, Wuhan University, Wuhan 430079 (China); Liu, Xin [School of Life Science and Technology, Huazhong University of Science and Technology, Wuhan 430074 (China)] [School of Life Science and Technology, Huazhong University of Science and Technology, Wuhan 430074 (China); Huang, Chi, E-mail: chihuang@whu.edu.cn [College of Chemistry and Molecular Sciences, Wuhan University, Wuhan 430072 (China)] [College of Chemistry and Molecular Sciences, Wuhan University, Wuhan 430072 (China)

    2012-08-15

    Highlights: ? Belt-like VO{sub 2}(A) with a rectangular cross section was synthesized. ? The formation mechanism of belt-like VO{sub 2}(A) was proposed. ? Belt-like VO{sub 2}(M) was prepared by the irreversible transformation of VO{sub 2}(A). ? VO{sub 2}(A) and VO{sub 2}(M) can be used as the optical switching materials. ? VO{sub 2}(A) and VO{sub 2}(M) have good oxidation resistance below 400 °C in air. -- Abstract: Belt-like VO{sub 2}(A) with a rectangular cross section (VA-RCS) was successfully synthesized using V{sub 2}O{sub 5}, H{sub 2}C{sub 2}O{sub 4}·2H{sub 2}O and H{sub 2}O as the starting materials by a facile hydrothermal approach. Some synthetic parameters, such as, the reaction time, reaction temperature and concentration of H{sub 2}C{sub 2}O{sub 4}·2H{sub 2}O, were systematically investigated to control the fabrication of belt-like VA-RCS. The formation mechanism of belt-like VA-RCS was proposed. Subsequently, belt-like VO{sub 2}(M) with a rectangular cross section (VM-RCS) was prepared by the irreversible transformation of VA-RCS at 700 °C for 2 h under the inert atmosphere. The phase transition temperature (T{sub c}) of VA-RCS and VM-RCS was evaluated by DSC test. The optical switching properties of VA-RCS and VM-RCS were studied by the variable-temperature infrared spectra, and it was found that the as-obtained VA-RCS and VM-RCS could be used as the optical switching materials. Furthermore, the oxidation resistance properties of VA-RCS and VM-RCS were investigated by TGA, indicating that they have good thermal stability and oxidation resistance below 400 °C in air.

  17. WHY SMALL IS BEAUTIFUL AND HOW TO DETECT ANOTHER 10 BILLION SMALL MAIN BELT ASTEROIDS. Henning Haack1

    E-Print Network [OSTI]

    Andersen, Anja C.

    WHY SMALL IS BEAUTIFUL ­ AND HOW TO DETECT ANOTHER 10 BILLION SMALL MAIN BELT ASTEROIDS. Henning. Introduction: Estimates of the size distribution of main belt asteroids suggest that there is a population- tant sub-kilometer asteroids in the main belt. Long intergration times cannot be used unless the object

  18. PUBLISHED ONLINE: 29 JANUARY 2012 | DOI: 10.1038/NPHYS2185 Explaining sudden losses of outer radiation belt

    E-Print Network [OSTI]

    Loss, Daniel

    of outer radiation belt electrons during geomagnetic storms Drew L. Turner1,2 *, Yuri Shprits1,2,3 , Michael Hartinger1 and Vassilis Angelopoulos1,2 The Van Allen radiation belts were first discovered in 1958 by the Explorer series of spacecraft1 . The dynamic outer belt consists primarily of relativistic

  19. Title: Prompt Creation of New Radiation Belts Cluster: Cross-Theme Theory and Data Analysis/SECTP

    E-Print Network [OSTI]

    Lotko, William

    Title: Prompt Creation of New Radiation Belts Cluster: Cross-Theme Theory and Data Analysis/SECTP Contributor: William Lotko/Dartmouth College · Radiation belt genesis via shock-induced magnetospheric compression The unexpected creation of new electron and proton radiation belts during the March 24, 1991

  20. ApJ, in press; this version: March 01, 2011 Secular resonance sweeping of the main asteroid belt during

    E-Print Network [OSTI]

    Malhotra, Renu

    ApJ, in press; this version: March 01, 2011 Secular resonance sweeping of the main asteroid belt a remnant asteroid belt to survive, we de- rive a lower limit on Saturn's migration speed of 0.15 AU My-1 during the era that the 6 resonance swept through the inner asteroid belt (semimajor axis range 2

  1. Bering a deep space mission to study the origin and evolution of the asteroid belt Philip Bidstrup1

    E-Print Network [OSTI]

    Andersen, Anja C.

    Bering ­ a deep space mission to study the origin and evolution of the asteroid belt Philip. An estimated population of approximately 1010 main belt asteroids in the size range 1 m to 1 km are too faint of the fragments are perturbed out of the main belt and fall on Earth as meteorites. The young surfaces and minimal

  2. Why do continents break-up parallel to ancient orogenic belts? A. Vauchez*, G. Barruol and A. Tommasi?

    E-Print Network [OSTI]

    Barruol, Guilhem

    Why do continents break-up parallel to ancient orogenic belts? A. Vauchez*, G. Barruol and A belts Ocean-opening through rifting and continent break-up is frequently related to the occurrence Atlantic oceans provide spectacularexamples of parallelism be- tween rifts and older orogenic belts

  3. to appear in Astrophysical Journal (Letters) An Analysis of the Statistics of the HST Kuiper Belt Object

    E-Print Network [OSTI]

    Brown, Michael E.

    to appear in Astrophysical Journal (Letters) An Analysis of the Statistics of the HST Kuiper Belt Belt objects in the HST data of Cochran et al. (1995), in which they report the discovery al. The detection of such a population of Halley­sized Kuiper Belt objects with these data

  4. 0036-1445/81.'"2301-0005 $01.00/0 f^MATICAL REMARKS ON THE VAN ALLEN RADIATION BELT

    E-Print Network [OSTI]

    Knill, Oliver

    0036-1445/81.'"2301-0005 $01.00/0 f^MATICAL REMARKS ON THE VAN ALLEN RADIATION BELT: A SURVEY radiation belt, were seemingly i vv j . {severai vears. sd, some of these particles were observed to have center or "adiabatic" approximation.) Under these circumstances, it was #12;THE VAN ALLEN RADIATION BELT

  5. hal-00193179,version1-4Dec2007 Origin of the Structure of the Kuiper Belt during a Dynamical

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    hal-00193179,version1-4Dec2007 Origin of the Structure of the Kuiper Belt during a Dynamical explore the origin and orbital evolution of the Kuiper belt in the frame- work of a recent model would stop migrating at its currently observed location. As a result, the Kuiper belt would have

  6. Tectonics of the Middle Triassic intracontinental Xuefengshan Belt, South China: new insights from structural and chronological constraints on the basal

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    1 Tectonics of the Middle Triassic intracontinental Xuefengshan Belt, South China: new insights-012-0780-5 #12;2 Abstract: In orogenic belts, a basal décollement zone often develops at depth to accommodate Xuefengshan Belt of South China, such a décollement zone is exposed in the core of anticlines formed

  7. P-and S-Wave Receiver Function Images of Crustal Imbrication beneath the Cheyenne Belt in Southeast Wyoming

    E-Print Network [OSTI]

    Dueker, Ken

    P- and S-Wave Receiver Function Images of Crustal Imbrication beneath the Cheyenne Belt estimation to constrain the crustal structure across the Archean­Proterozoic Cheyenne belt suture of Proterozoic lower crust across the Chey- enne belt. Both P and S-wave receiver function images delineate

  8. Title: Prompt Creation of New Radiation Belts Cluster: Cross-Theme Theory and Data Analysis/SECTP

    E-Print Network [OSTI]

    Lotko, William

    Title: Prompt Creation of New Radiation Belts Cluster: Cross-Theme Theory and Data Analysis-pushing code for radiation belt particles in a global MHD simulation of the solar wind/SECTP Contributor: William Lotko/Dartmouth College · Radiation belt genesis via shock-induced magnetospheric

  9. EDUCATION HISTORY 2001-M.Sc. in Geological Sciences, University of Roma Tre

    E-Print Network [OSTI]

    -and-thrust belts (Apennines, Pyrenees, Zagros) by organic and inorganic thermal indicators; Correlation of clay

  10. MAIN-BELT COMET P/2012 T1 (PANSTARRS)

    SciTech Connect (OSTI)

    Hsieh, Henry H.; Kaluna, Heather M.; Yang Bin; Haghighipour, Nader; Micheli, Marco; Denneau, Larry; Jedicke, Robert; Kleyna, Jan; Veres, Peter; Wainscoat, Richard J.; Ansdell, Megan; Elliott, Garrett T.; Keane, Jacqueline V.; Meech, Karen J.; Riesen, Timm E.; Sonnett, Sarah; Novakovic, Bojan; Fitzsimmons, Alan; Moskovitz, Nicholas A.; Sheppard, Scott S.; and others

    2013-07-01

    We present initial results from observations and numerical analyses aimed at characterizing the main-belt comet P/2012 T1 (PANSTARRS). Optical monitoring observations were made between 2012 October and 2013 February using the University of Hawaii 2.2 m telescope, the Keck I telescope, the Baade and Clay Magellan telescopes, Faulkes Telescope South, the Perkins Telescope at Lowell Observatory, and the Southern Astrophysical Research Telescope. The object's intrinsic brightness approximately doubles from the time of its discovery in early October until mid-November and then decreases by {approx}60% between late December and early February, similar to photometric behavior exhibited by several other main-belt comets and unlike that exhibited by disrupted asteroid (596) Scheila. We also used Keck to conduct spectroscopic searches for CN emission as well as absorption at 0.7 {mu}m that could indicate the presence of hydrated minerals, finding an upper limit CN production rate of Q{sub CN} < 1.5 Multiplication-Sign 10{sup 23} mol s{sup -1}, from which we infer a water production rate of Q{sub H{sub 2O}}<5 Multiplication-Sign 10{sup 25} mol s{sup -1}, and no evidence of the presence of hydrated minerals. Numerical simulations indicate that P/2012 T1 is largely dynamically stable for >100 Myr and is unlikely to be a recently implanted interloper from the outer solar system, while a search for potential asteroid family associations reveals that it is dynamically linked to the {approx}155 Myr old Lixiaohua asteroid family.

  11. HIGH ECLIPTIC LATITUDE SURVEY FOR SMALL MAIN-BELT ASTEROIDS

    SciTech Connect (OSTI)

    Terai, Tsuyoshi [National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Takahashi, Jun; Itoh, Yoichi, E-mail: tsuyoshi.terai@nao.ac.jp [Center for Astronomy, University of Hyogo, 407-2 Nishigaichi, Sayo-cho, Sayo-gun, Hyogo 679-5313 (Japan)

    2013-11-01

    Main-belt asteroids have been continuously colliding with one another since they were formed. Their size distribution is primarily determined by the size dependence of asteroid strength against catastrophic impacts. The strength scaling law as a function of body size could depend on collision velocity, but the relationship remains unknown, especially under hypervelocity collisions comparable to 10 km s{sup –1}. We present a wide-field imaging survey at an ecliptic latitude of about 25° for investigating the size distribution of small main-belt asteroids that have highly inclined orbits. The analysis technique allowing for efficient asteroid detections and high-accuracy photometric measurements provides sufficient sample data to estimate the size distribution of sub-kilometer asteroids with inclinations larger than 14°. The best-fit power-law slopes of the cumulative size distribution are 1.25 ± 0.03 in the diameter range of 0.6-1.0 km and 1.84 ± 0.27 in 1.0-3.0 km. We provide a simple size distribution model that takes into consideration the oscillations of the power-law slope due to the transition from the gravity-scaled regime to the strength-scaled regime. We find that the high-inclination population has a shallow slope of the primary components of the size distribution compared to the low-inclination populations. The asteroid population exposed to hypervelocity impacts undergoes collisional processes where large bodies have a higher disruptive strength and longer lifespan relative to tiny bodies than the ecliptic asteroids.

  12. 1216 IEEE TRANSACTIONS ON ROBOTICS, VOL. 28, NO. 6, DECEMBER 2012 Kinematic Condition for Maximizing the Thrust

    E-Print Network [OSTI]

    Kim, Ho-Young

    perfor- mance than that of screw propulsion [1]. Various mechanisms using multilinks have been developed.ac.kr; kjcho@snu.ac.kr). J. Lee and H.-Y. Kim are with the Micro Fluid Mechanics Laboratory, School the condition for maximizing the thrust generated by a compliant fin propulsion system. When a fin oscil- lates

  13. RADIATION BELTS AND SUBSTORM PARTICLE INJECTIONS Department of Aerospace Engineering Sciences and LASP, University of Colorado, Boulder, CO 80303-7814, USA

    E-Print Network [OSTI]

    Li, Xinlin

    1 RADIATION BELTS AND SUBSTORM PARTICLE INJECTIONS Xinlin Li Department of Aerospace Engineering belt particles in the Earth's magnetosphere is briefly reviewed, with a focus on the radiation belt energies are presented and the acceleration mecha- nisms for radiation belt electrons are discussed. 1

  14. Evaluation of the orogenic belt hypothesis for the formation of the Thaumasia Highlands, Mars

    E-Print Network [OSTI]

    , 2002, Borraccini et al., 2007] or continentalscale salt tectonics [Montgomery et al., 2009; Dohm et al., 2001], an orogenic belt produced by an ancient period of plate tectonics or large scale

  15. Migration of matter from the Edgeworth-Kuiper and main asteroid belts to the Earth

    E-Print Network [OSTI]

    S. I. Ipatov

    2002-05-16

    A considerable portion of near-Earth objects could have come from the trans-Neptunian belt. Some of them have aphelia deep inside Jupiter's orbit during more than 1 Myr.

  16. Shaping mobile belts by small-scale convection Claudio Faccenna1,2

    E-Print Network [OSTI]

    Becker, Thorsten W.

    ­Dinarides­Hellenides, and further to the east joining the Bitlis­Zagros zone. Most of these fast anomalies are not connected). For example, the collision along the Zagros­Bitlis belt induced the westward motion of Anatolia

  17. The Electric Field and Waves Instruments on the Radiation Belt Storm Probes Mission

    E-Print Network [OSTI]

    Wygant, J. R.

    The Electric Fields and Waves (EFW) Instruments on the two Radiation Belt Storm Probe (RBSP) spacecraft (recently renamed the Van Allen Probes) are designed to measure three dimensional quasi-static and low frequency ...

  18. De-biased populations of Kuiper Belt objects from the Deep Ecliptic Survey

    E-Print Network [OSTI]

    Adams, Elisabeth Rose

    The Deep Ecliptic Survey (DES) was a survey project that discovered hundreds of Kuiper Belt objects from 1998 to 2005. Extensive follow-up observations of these bodies has yielded 304 objects with well-determined orbits ...

  19. Water Ice on the Satellite of Kuiper Belt Object 2003 EL61

    E-Print Network [OSTI]

    K. M Barkume; M. E. Brown; E. L. Schaller

    2006-01-24

    We have obtained a near infrared spectrum of the brightest satellite of the large Kuiper Belt Object, 2003 EL61. The spectrum has absorption features at 1.5 and 2.0 microns, indicating that water ice is present on the surface. We find that the satellite's absorption lines are much deeper than water ice features typically found on Kuiper Belt Objects. We argue that the unusual spectrum indicates that the satellite was likely formed by impact and not by capture.

  20. Mechanical characteristics of folds in Upper Cretaceous strata in the Disturbed Belt of northwestern Montana 

    E-Print Network [OSTI]

    Gilbert, Pat Kader

    1974-01-01

    MECHANICAL CHARACTERISTICS OF FOLDS IN UPPER CRETACEOUS STRATA IN THE DISTURBED BELT OF NORTHWESTERN MONTANA A Thesis by PAT KADER GILBERT Submitted to the Graduate College of Texas A&M University in partial fulfillment of the requirements... for the degree of MASTER OF SCIENCE May 1974 Major Subject: Geology MECHANICAL CHARACTERISTICS OF FOLDS IN UPPER CRETACEOUS STRATA IN THE DISTURBED BELT OF NORTHWESTERN MONTANA A Thesis by PAT KADER GILBERT Approved as to style and content by: (Chairman...

  1. The absolute magnitude distribution of Kuiper Belt objects

    SciTech Connect (OSTI)

    Fraser, Wesley C. [Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7 (Canada); Brown, Michael E. [Division of Geological and Planetary Sciences, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125 (United States); Morbidelli, Alessandro [Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d'Azur, BP 4229, F-06304 Nice (France); Parker, Alex [Department of Astronomy, University of California at Berkeley, Berkeley, CA 94720 (United States); Batygin, Konstantin, E-mail: wesley.fraser@nrc.ca [Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 51, Cambridge, MA 02138 (United States)

    2014-02-20

    Here we measure the absolute magnitude distributions (H-distribution) of the dynamically excited and quiescent (hot and cold) Kuiper Belt objects (KBOs), and test if they share the same H-distribution as the Jupiter Trojans. From a compilation of all useable ecliptic surveys, we find that the KBO H-distributions are well described by broken power laws. The cold population has a bright-end slope, ?{sub 1}=1.5{sub ?0.2}{sup +0.4}, and break magnitude, H{sub B}=6.9{sub ?0.2}{sup +0.1} (r'-band). The hot population has a shallower bright-end slope of, ?{sub 1}=0.87{sub ?0.2}{sup +0.07}, and break magnitude H{sub B}=7.7{sub ?0.5}{sup +1.0}. Both populations share similar faint-end slopes of ?{sub 2} ? 0.2. We estimate the masses of the hot and cold populations are ?0.01 and ?3 × 10{sup –4} M {sub ?}. The broken power-law fit to the Trojan H-distribution has ?{sub 1} = 1.0 ± 0.2, ?{sub 2} = 0.36 ± 0.01, and H {sub B} = 8.3. The Kolmogorov-Smirnov test reveals that the probability that the Trojans and cold KBOs share the same parent H-distribution is less than 1 in 1000. When the bimodal albedo distribution of the hot objects is accounted for, there is no evidence that the H-distributions of the Trojans and hot KBOs differ. Our findings are in agreement with the predictions of the Nice model in terms of both mass and H-distribution of the hot and Trojan populations. Wide-field survey data suggest that the brightest few hot objects, with H{sub r{sup ?}}?3, do not fall on the steep power-law slope of fainter hot objects. Under the standard hierarchical model of planetesimal formation, it is difficult to account for the similar break diameters of the hot and cold populations given the low mass of the cold belt.

  2. COLOR DEPENDENCE IN THE SIZE DISTRIBUTION OF MAIN BELT ASTEROIDS REVISITED

    SciTech Connect (OSTI)

    August, Tyler M.; Wiegert, Paul A.

    2013-06-15

    The size distribution of the asteroid belt is examined with 16956 main belt asteroids detected in data taken from the Canada-France-Hawaii Telescope Legacy Survey in two filters (g' and r'). The cumulative H (absolute magnitude) distribution is examined in both filters, and both match well to simple power laws down to H = 17, with slopes in rough agreement with those reported the literature. This implies that disruptive collisions between asteroids are gravitationally dominated down to at least this size, and probably sub-kilometer scales. The slopes of these distributions appear shallower in the outer belt than the inner belt, and the g' distributions appear slightly steeper than the r'. The slope shallowing in the outer belt may reflect a real compositional difference: the inner asteroid belt has been suggested to consist mostly of stony and/or metallic S-type asteroids, whereas carbonaceous C-types are thought to be more prevalent further from the Sun. No waves are seen in the size distribution above H = 15. Since waves are expected to be produced at the transition from gravitationally-dominated to internal strength-dominated collisions, their absence here may imply that the transition occurs at sub-kilometer scales, much smaller than the H = 17 (diameter {approx} 1.6 km) cutoff of this study.

  3. Biomechanical caracterisation of lumbar belt by full-field techniques: Preliminary results

    E-Print Network [OSTI]

    Bonnaire, Rebecca; Calmels, Paul; Convert, Reynald

    2013-01-01

    In France, 50% of the population per year is suffering from low back pain. Lumbar belt are frequently proposed as a part of the treatment of this pathology. However mechanical ways of working of this medical device is not clearly understood, but abdominal pressure is often related. So an optical method was developed in this study to measure strain in lumbar belt and trunk interface and to derive a pressure estimation. Optical method consisted of coupling fringe projection and digital image correlation (DIC). Measurement has been carried out on the right side of a manikin wearing a lumbar belt. Average strain is 0.2 and average pressure is 1 kPa. Continuation of this study will be comparison of strain and pressure in different areas of lumbar belt (left side, front and back) and comparison of different lumbar belts. Results will be used in a finite elements model to determine lumbar belt impact in intern body. In long term, this kind of study will be done on human.

  4. Non-Perturbative Contribution to the Thrust Distribution in $e^+ e^-$ Annihilation

    E-Print Network [OSTI]

    R. A. Davison; B. R. Webber

    2008-11-18

    We re-evaluate the non-perturbative contribution to the thrust distribution in $e^+e^-\\to$ hadrons, in the light of the latest experimental data and the recent NNLO perturbative calculation of this quantity. By extending the calculation to NNLO+NLL accuracy, we perform the most detailed study to date of the effects of non-perturbative physics on this observable. In particular, we investigate how well a model based on a low-scale QCD effective coupling can account for such effects. We find that the difference between the improved perturbative distribution and the experimental data is consistent with a $1/Q$-dependent non-perturbative shift in the distribution, as predicted by the effective coupling model. Best fit values of $\\alpha_s(M_Z) = 0.1164^{+0.0028}_{-0.0026}$ and $\\alpha_0(2 GeV)=0.59+/-0.03$ are obtained with $\\chi^2/d.o.f.=1.09$. This is consistent with NLO+NLL results but the quality of fit is improved. The agreement in $\\alpha_0$ is non-trivial because a part of the 1/Q-dependent contribution (the infrared renormalon) is included in the NNLO perturbative correction.

  5. Volatile Loss and Classification of Kuiper Belt Objects

    E-Print Network [OSTI]

    Johnson, R E; Young, L A; Volkov, A N; Schmidt, C

    2015-01-01

    Observations indicate that some of the largest Kuiper Belt Objects (KBOs) have retained volatiles in the gas phase, which implies the presence of an atmosphere that can affect their reflectance spectra and thermal balance. Volatile escape rates driven by solar heating of the surface were estimated by Schaller and Brown (2007) (SB) and Levi and Podolak (2009)(LP) using Jeans escape from the surface and a hydrodynamic model respectively. Based on recent molecular kinetic simulations these rates can be hugely in error (e.g., a factor of $\\sim 10^{16}$ for the SB estimate for Pluto). In this paper we estimate the loss of primordial N$_2$ for several large KBOs guided by recent molecular kinetic simulations of escape due to solar heating of the surface and due to UV/EUV heating of the upper atmosphere. For the latter we extrapolate simulations of escape from Pluto (Erwin et al. 2013) using the energy limited escape model recently validated for the KBOs of interest by molecular kinetic simulations (Johnson et al. 2...

  6. Planar resonant periodic orbits in Kuiper belt dynamics

    E-Print Network [OSTI]

    George Voyatzis; Thomas Kotoulas

    2005-02-28

    In the framework of the planar restricted three body problem we study a considerable number of resonances associated to the Kuiper Belt dynamics and located between 30 and 48 a.u. Our study is based on the computation of resonant periodic orbits and their stability. Stable periodic orbits are surrounded by regular librations in phase space and in such domains the capture of trans-Neptunian object is possible. All the periodic orbits found are symmetric and there is evidence for the existence of asymmetric ones only in few cases. In the present work first, second and third order resonances are under consideration. In the planar circular case we found that most of the periodic orbits are stable. The families of periodic orbits are temporarily interrupted by collisions but they continue up to relatively large values of the Jacobi constant and highly eccentric regular motion exists for all cases. In the elliptic problem and for a particular eccentricity value of the primary bodies the periodic orbits are isolated. The corresponding families, where they belong to, bifurcate from specific periodic orbits of the circular problem and seem to continue up to the rectilinear problem. Both stable and unstable orbits are obtained for each case. In the elliptic problem the unstable orbits found are associated with narrow chaotic domains in phase space. The evolution of the orbits, which are located in such chaotic domains, seems to be practically regular and bounded for long time intervals.

  7. First results from the Herschel Gould Belt Survey in Taurus

    E-Print Network [OSTI]

    Kirk, J M; Palmeirim, P; Andre, Ph; Griffin, M J; Hargrave, P J; Konyves, V; Bernard, J P; Nutter, D J; Sibthorpe, B; Di Francesco, J; Abergel, A; Arzoumanian, D; Benedettini, M; Bontemps, S; Elia, D; Hennemann, M; Hill, T; Men'shchikov, A; Motte, F; Nguyen-Luong, Q; Peretto, N; Pezzuto, S; Rygl, K L J; Sadavoy, S I; Schisano, E; Schneider, N; Testi, L; White, G

    2013-01-01

    The whole of the Taurus region (a total area of 52 sq. deg.) has been observed by the Herschel SPIRE and PACS instruments at wavelengths of 70, 160, 250, 350 and 500 {\\mu}m as part of the Herschel Gould Belt Survey. In this paper we present the first results from the part of the Taurus region that includes the Barnard 18 and L1536 clouds. A new source-finding routine, the Cardiff Source-finding AlgoRithm (CSAR), is introduced, which is loosely based on CLUMPFIND, but that also generates a structure tree, or dendrogram, which can be used to interpret hierarchical clump structure in a complex region. Sources were extracted from the data using the hierarchical version of CSAR and plotted on a mass-size diagram. We found a hierarchy of objects with sizes in the range 0.024-2.7 pc. Previous studies showed that gravitationally bound prestellar cores and unbound starless clumps appeared in different places on the mass-size diagram. However, it was unclear whether this was due to a lack of instrumental dynamic range ...

  8. Initial highlights from the Herschel Gould Belt survey

    E-Print Network [OSTI]

    André, Ph; Bontemps, S; Könyves, V; Motte, F; Schneider, N; Didelon, P; Minier, V; Saraceno, P; Ward-Thompson, D; Di Francesco, J; White, G; Molinari, S; Testi, L; Abergel, A; Griffin, M; Henning, Th; Royer, P; Merín, B; Vavrek, R; Attard, M; Arzoumanian, D; Wilson, C D; Ade, P; Aussel, H; Baluteau, J -P; Benedettini, M; Bernard, J -Ph; Blommaert, J A D L; Cambrésy, L; Cox, P; Di Giorgio, A; Hargrave, P; Hennemann, M; Huang, M; Kirk, J; Krause, O; Launhardt, R; Leeks, S; Pennec, J Le; Li, J Z; Martin, P; Maury, A; Olofsson, G; Omont, A; Peretto, N; Pezzuto, S; Prusti, T; Roussel, H; Russeil, D; Sauvage, M; Sibthorpe, B; Sicilia-Aguilar, A; Spinoglio, L; Waelkens, C; Woodcraft, A; Zavagno, A

    2010-01-01

    We summarize the first results from the Gould Belt survey, obtained toward the Aquila Rift and Polaris Flare regions during the 'science demonstration phase' of Herschel. Our 70-500 micron images taken in parallel mode with the SPIRE and PACS cameras reveal a wealth of filamentary structure, as well as numerous dense cores embedded in the filaments. Between ~ 350 and 500 prestellar cores and ~ 45-60 Class 0 protostars can be identified in the Aquila field, while ~ unbound starless cores and no protostars are observed in the Polaris field. The prestellar core mass function (CMF) derived for the Aquila region bears a strong resemblance to the stellar initial mass function (IMF), already confirming the close connection between the CMF and the IMF with much better statistics than earlier studies. Comparing and contrasting our Herschel results in Aquila and Polaris, we propose an observationally-driven scenario for core formation according to which complex networks of long, thin filaments form first within molecul...

  9. The Gould Belt 'MISFITS' Survey: The Real Solar Neighborhood Protostars

    E-Print Network [OSTI]

    Heiderman, Amanda

    2015-01-01

    We present an HCO$^{+}$ J=3-2 survey of Class 0+I and Flat SED young stellar objects (YSOs) found in the Gould Belt clouds by surveys with Spitzer. Our goal is to provide a uniform Stage 0+I source indicator for these embedded protostar candidates. We made single point HCO$^{+}$ J = 3-2 measurements toward the source positions at the CSO and APEX of 546 YSOs (89% of the Class 0+I + Flat SED sample). Using the criteria from van Kempen et al. (2009), we classify sources as Stage 0+I or bona fide protostars and find that 84% of detected sources meet the criteria. We recommend a timescale for the evolution of Stage 0+I (embedded protostars) of 0.54 Myr. We find significant correlations of HCO$^{+}$ integrated intensity with ${\\alpha}$ and $T_{bol}$ but not with $L_{bol}$. The detection fraction increases smoothly as a function of ${\\alpha}$ and $L_{bol}$, while decreasing smoothly with $T_{bol}$. Using the Stage 0+I sources tightens the relation between protostars and high extinction regions of the cloud; 89% of ...

  10. Kuiper belt structure around nearby super-Earth host stars

    E-Print Network [OSTI]

    Kennedy, Grant M; Marmier, Maxime; Greaves, Jane S; Wyatt, Mark C; Bryden, Geoffrey; Holland, Wayne; Lovis, Christophe; Matthews, Brenda C; Pepe, Francesco; Sibthorpe, Bruce; Udry, Stéphane

    2015-01-01

    We present new observations of the Kuiper belt analogues around HD 38858 and HD 20794, hosts of super-Earth mass planets within 1 au. As two of the four nearby G-type stars (with HD 69830 and 61 Vir) that form the basis of a possible correlation between low-mass planets and debris disc brightness, these systems are of particular interest. The disc around HD 38858 is well resolved with Herschel and we constrain the disc geometry and radial structure. We also present a probable JCMT sub-mm continuum detection of the disc and a CO J=2-1 upper limit. The disc around HD 20794 is much fainter and appears marginally resolved with Herschel, and is constrained to be less extended than the discs around 61 Vir and HD 38858. We also set limits on the radial location of hot dust recently detected around HD 20794 with near-IR interferometry. We present HARPS upper limits on unseen planets in these four systems, ruling out additional super-Earths within a few au, and Saturn-mass planets within 10 au. We consider the disc st...

  11. MAIN-BELT COMET 238P/READ REVISITED

    SciTech Connect (OSTI)

    Hsieh, Henry H.; Meech, Karen J.; Pittichova, Jana, E-mail: hsieh@ifa.hawaii.edu, E-mail: meech@ifa.hawaii.edu, E-mail: jana@ifa.hawaii.edu [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States)

    2011-07-20

    We present a series of observations of the return of activity in main-belt comet (MBC) 238P/Read. Using data obtained in 2010 July and August when 238P appeared to be largely inactive, we find best-fit IAU phase function parameters of H = 19.05 {+-} 0.05 mag, corresponding to a nucleus radius of r{sub n} {approx} 0.4 km (assuming an albedo of p{sub R} = 0.05), and G = -0.03 {+-} 0.05. Observations from 2010 September onward show a clear rise in activity, causing both a notable change in visible morphology and increasing photometric excesses beyond what would be expected based on bare nucleus observations. By the end of the observing period reported on here, the dust mass in the coma shows indications of reaching a level comparable to that observed in 2005, but further observations are highly encouraged once 238P again becomes observable from Earth in mid-2011 to confirm whether this level of activity is achieved, or if the comet shows a noticeable drop in activity strength compared with 2005. Comet 238P is now the second MBC (after 133P/Elst-Pizarro) observed to exhibit recurrent activity, providing strong corroboration for the conclusion that it is a true comet whose active episodes are driven by sublimation of volatile ice.

  12. Dynamical implantation of objects in the Kuiper Belt

    SciTech Connect (OSTI)

    Brasil, P. I. O.

    2014-09-01

    Several models have been suggested in the past to describe the dynamical formation of hot Kuiper Belt objects (hereafter Hot Classicals or HCs for short). Here, we discuss a dynamical mechanism that allows orbits to evolve from the primordial planetesimal disk at ? 35 AU to reach the orbital region now occupied by HCs. We performed three different sets of numerical simulations to illustrate this mechanism. Two of these simulations were based on modern theories for the early evolution of the solar system (the Nice and jumping-Jupiter models). The third simulation was performed with the purpose of increasing the resolution at 41-46 AU. The common aspect of these simulations is that Neptune scatters planetesimals from ? 35 AU to >40 AU and then undergoes a long phase of slow residual migration. Our results show that to reach an HC orbit, a scattered planetesimal needs to be captured in a mean motion resonance (MMR) with Neptune where the perihelion distance rises due to the Kozai resonance (which occurs in MMRs even for moderate inclinations). Finally, while Neptune is still migrating, the planetesimal is released from the MMR on a stable HC orbit. We show that the orbital distribution of HCs expected from this process provides a reasonable match to observations. The capture efficiency and the mass deposited into the HC region appears to be sensitive to the maximum eccentricity reached by Neptune during the planetary instability phase. Additional work will be needed to resolve this dependency in detail.

  13. International perspectives on coal preparation

    SciTech Connect (OSTI)

    1997-12-31

    The report consists of the vugraphs from the presentations which covered the following topics: Summaries of the US Department of Energy`s coal preparation research programs; Preparation trends in Russia; South African coal preparation developments; Trends in hard coal preparation in Germany; Application of coal preparation technology to oil sands extraction; Developments in coal preparation in China; and Coal preparation in Australia.

  14. Conceptual Engine System Design for NERVA derived 66.7KN and 111.2KN Thrust Nuclear Thermal Rockets

    SciTech Connect (OSTI)

    Fittje, James E. [Analex Corporation, Cleveland Ohio (United States); Buehrle, Robert J. [NASA Glenn Research Center, Brookpark Ohio 44135 (United States)

    2006-01-20

    The Nuclear Thermal Rocket concept is being evaluated as an advanced propulsion concept for missions to the moon and Mars. A tremendous effort was undertaken during the 1960's and 1970's to develop and test NERVA derived Nuclear Thermal Rockets in the 111.2 KN to 1112 KN pound thrust class. NASA GRC is leveraging this past NTR investment in their vehicle concepts and mission analysis studies, and has been evaluating NERVA derived engines in the 66.7 KN to the 111.2 KN thrust range. The liquid hydrogen propellant feed system, including the turbopumps, is an essential component of the overall operation of this system. The NASA GRC team is evaluating numerous propellant feed system designs with both single and twin turbopumps. The Nuclear Engine System Simulation code is being exercised to analyze thermodynamic cycle points for these selected concepts. This paper will present propellant feed system concepts and the corresponding thermodynamic cycle points for 66.7 KN and 111.2 KN thrust NTR engine systems. A pump out condition for a twin turbopump concept will also be evaluated, and the NESS code will be assessed against the Small Nuclear Rocket Engine preliminary thermodynamic data.

  15. The Insignificance of P-R Drag in Detectable Extrasolar Planetesimal Belts

    E-Print Network [OSTI]

    M. C. Wyatt

    2005-01-04

    This paper considers a simple model in which dust produced in a planetesimal belt migrates in toward the star due to P-R drag suffering destructive collisions with other dust grains on the way. Assuming the dust is all of the same size, the resulting surface density distribution can be derived analytically and depends only on the parameter eta0=5000tau*sqrt(Mstar/r)/beta; this parameter can be determined observationally with the hypothesis that beta=0.5. For massive belts in which eta0>>1 dust is confined to the planetesimal belt, while the surface density of more tenuous belts, in which eta0belts at different distances from different mass stars shows that the dust belts which have been detected to date should have eta0>>1; dust belts with eta010. This means that these disks are so massive that mutual collisions prevent dust from reaching the inner regions of these systems and P-R drag can be ignored when studying their dynamics. Models for the formation of structure in debris disks by the trapping of particles into planetary resonances by P-R drag should be reconsidered. However, since collisions do not halt 100% of the dust, this means that in the absence of planetary companions debris disk systems should be populated by small quantities of hot dust which may be detectable in the mid-IR. Even in disks with eta0<<1 the temperature of dust emission is shown to be a reliable tracer of the planetesimal distribution meaning that inner holes in the dust distribution imply a lack of colliding planetesimals in the inner regions.

  16. JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 88, NO. B9, PAGES 7429-7448, SEPTEMBER 10,1983 --BACK ARC THRUSTING IN THE EASTERN SUNDA ARC, INDONESIA

    E-Print Network [OSTI]

    McCaffrey, Robert

    THRUSTING IN THE EASTERN SUNDA ARC, INDONESIA: A CONSEQUENCE OF ARC-CONTINENT COLLISION Eli A. Silver Center, Jalan Diponegoro 57, Bandung, Indonesia Abstract. The structure of the eastern Sunda convergence

  17. ORBITS, MASSES, AND EVOLUTION OF MAIN BELT TRIPLE (87) SYLVIA

    SciTech Connect (OSTI)

    Fang, Julia; Margot, Jean-Luc [Department of Physics and Astronomy, University of California, Los Angeles, CA 90095 (United States); Rojo, Patricio [Departamento de Astronomia, Universidad de Chile, Santiago (Chile)

    2012-08-15

    Sylvia is a triple asteroid system located in the main belt. We report new adaptive optics observations of this system that extend the baseline of existing astrometric observations to a decade. We present the first fully dynamical three-body model for this system by fitting to all available astrometric measurements. This model simultaneously fits for individual masses, orbits, and primary oblateness. We find that Sylvia is composed of a dominant central mass surrounded by two satellites orbiting at 706.5 {+-} 2.5 km and 1357 {+-} 4.0 km, i.e., about 5 and nearly 10 primary radii. We derive individual masses of 1.484{sup +0.016}{sub -0.014} Multiplication-Sign 10{sup 19} kg for the primary (corresponding to a density of 1.29 {+-} 0.39 g cm{sup -3}), 7.33{sup +4.7}{sub -2.3} Multiplication-Sign 10{sup 14} kg for the inner satellite, and 9.32{sup +20.7}{sub -8.3} Multiplication-Sign 10{sup 14} kg for the outer satellite. The oblateness of the primary induces substantial precession and the J{sub 2} value can be constrained to the range of 0.0985-0.1. The orbits of the satellites are relatively circular with eccentricities less than 0.04. The spin axis of the primary body and the orbital poles of both satellites are all aligned within about 2 deg of each other, indicating a nearly coplanar configuration and suggestive of satellite formation in or near the equatorial plane of the primary. We also investigate the past orbital evolution of the system by simulating the effects of a recent passage through 3:1 mean-motion eccentricity-type resonances. In some scenarios this allow us to place constraints on interior structure and past eccentricities.

  18. Laramide thrusting and Tertiary deformation Tierra Caliente, Michoacan and Guerrero States, southwestern Mexico

    SciTech Connect (OSTI)

    Johnson, C.A.; Harrison, C.G.A. ); Lang, H. ); Barros, J.A.; Cabral-Cano, E.

    1990-05-01

    Field investigations and detailed interpretations of Landsat Thematic Mapper images are in progress to improve understanding of regional structure and tectonics of the southernmost extension of the North American cordillera. Two areas have been selected within the Ciudad Altamirano 1:250,000 topographical sheet for geologic mapping and structural interpretation at 1:50,000 scale. The authors results to date require modification of previous ideas concerning the style and timing of deformations, the role and timing of terrane accretion in the overall tectonic history of the region, and the importance of southern Mexico to investigations of the tectonic evolution of the plates in the region. The relative sequence of deformation in the area correlates well with variations in relative motion between North America and plates in the Pacific. Post-Campanian thrusts and generally eastward-verging folds deformed the Mesozoic sequence during the (Laramide equivalent) Hidalgoan orogeny, associated with high-velocity east-west convergence with the Farallon plate that began about 70 Ma. The resulting unconformity was covered by the Tertiary Balsas Formation, a thick sequence of mostly continental clastics. The Tertiary stratigraphy is regionally and sometimes locally variable, but it can be divided into two members. The lower member is relatively volcanic poor and more deformed, and it lies below a regionally significant mid-Tertiary unconformity, which may mark a change to northeast-directed convergence with the Farallon plate sometime prior to 40 Ma. Continued mid-Tertiary deformation in southern Mexico may be related to eastward movement of the Chortis block and the resulting truncation of the Pacific margin of Mexico. The authors also suggest a tentative correlation between the volcaniclastic member of the Lower Cretaceous San Lucas Formation and the protolith of the Roca Verde metamorphics to the east.

  19. THE SURFACE COMPOSITION OF LARGE KUIPER BELT OBJECT 2007 OR10

    SciTech Connect (OSTI)

    Brown, M. E.; Fraser, W. C. [Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125 (United States); Burgasser, A. J., E-mail: aburgasser@ucsd.edu [Center for Astrophysics and Space Science, University of California San Diego, La Jolla, CA 92093 (United States)

    2011-09-10

    We present photometry and spectra of the large Kuiper belt object 2007 OR10. The data show significant near-infrared absorption features due to water ice. While most objects in the Kuiper belt with water ice absorption this prominent have the optically neutral colors of water ice, 2007 OR10 is among the reddest Kuiper belt objects known. One other large Kuiper belt object-Quaoar-has similar red coloring and water ice absorption, and it is hypothesized that the red coloration of this object is due to irradiation of the small amounts of methane able to be retained on Quaoar. 2007 OR10, though warmer than Quaoar, is in a similar volatile retention regime because it is sufficiently larger that its stronger gravity can still retain methane. We propose, therefore, that the red coloration on 2007 OR10 is also caused by the retention of small amounts of methane. Positive detection of methane on 2007 OR10 will require spectra with higher signal to noise. Models for volatile retention on Kuiper belt objects appear to continue to do an excellent job reproducing all of the available observations.

  20. MAIN BELT ASTEROIDS WITH WISE/NEOWISE. I. PRELIMINARY ALBEDOS AND DIAMETERS

    SciTech Connect (OSTI)

    Masiero, Joseph R.; Mainzer, A. K.; Bauer, J. M.; Eisenhardt, P. R. M.; DeBaun, E.; Elsbury, D.; Gautier, T. IV; Gomillion, S.; Wilkins, A. [Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA 91109 (United States); Grav, T. IV [Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 (United States); Cutri, R. M.; Dailey, J. [Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125 (United States); McMillan, R. S. [Lunar and Planetary Laboratory, University of Arizona, Kuiper Space Science Building 92, Tucson, AZ 85721-0092 (United States); Spahr, T. B. [Minor Planet Center, Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States); Skrutskie, M. F. [Department of Astronomy, University of Virginia, Charlottesville, VA 22903-0818 (United States); Tholen, D. [Institute for Astronomy, University of Hawaii, Honolulu, HI 96822 (United States); Walker, R. G. [Monterey Institute for Research in Astronomy, Monterey, CA (United States); Wright, E. L., E-mail: Joseph.Masiero@jpl.nasa.gov [UCLA Astronomy, Los Angeles, CA 90095-1547 (United States)

    2011-11-10

    We present initial results from the Wide-field Infrared Survey Explorer (WISE), a four-band all-sky thermal infrared survey that produces data well suited for measuring the physical properties of asteroids, and the NEOWISE enhancement to the WISE mission allowing for detailed study of solar system objects. Using a NEATM thermal model fitting routine, we compute diameters for over 100,000 Main Belt asteroids from their IR thermal flux, with errors better than 10%. We then incorporate literature values of visible measurements (in the form of the H absolute magnitude) to determine albedos. Using these data we investigate the albedo and diameter distributions of the Main Belt. As observed previously, we find a change in the average albedo when comparing the inner, middle, and outer portions of the Main Belt. We also confirm that the albedo distribution of each region is strongly bimodal. We observe groupings of objects with similar albedos in regions of the Main Belt associated with dynamical breakup families. Asteroid families typically show a characteristic albedo for all members, but there are notable exceptions to this. This paper is the first look at the Main Belt asteroids in the WISE data, and only represents the preliminary, observed raw size, and albedo distributions for the populations considered. These distributions are subject to survey biases inherent to the NEOWISE data set and cannot yet be interpreted as describing the true populations; the debiased size and albedo distributions will be the subject of the next paper in this series.

  1. Preparation of acetaldehyde

    DOE Patents [OSTI]

    Tustin, G.C.; Depew, L.S.

    1997-10-21

    Disclosed is a process for the preparation of acetaldehyde by the hydrogenation of ketene in the presence of a transition metal hydrogenation catalyst.

  2. Using Intermediate-Luminosity Optical Transients (ILOTs) to reveal extended exo-solar Kuiper belt objects

    E-Print Network [OSTI]

    Bear, Ealeal

    2016-01-01

    We suggest that in the rare case of an Intermediate-Luminosity Optical Transient (ILOTs) event, evaporation of exo-solar Kuiper belt objects (ExoKBOs) at distances of d~500 - 10000AU from the ILOT can be detected. If the ILOT lasts for 1 month to a few years, enough dust might be ejected from the ExoKBOs for the IR emission to be detected. Because of the large distance of the ExoKBOs, tens of years will pass before the ILOT wind disperses the dust. We suggest that after an ILOT outburst there is a period of months to several years during which IR excess emission might hint at the existence of a Kuiper belt analog (ExoK-Belt).

  3. A RESOLVED MILLIMETER EMISSION BELT IN THE AU Mic DEBRIS DISK

    SciTech Connect (OSTI)

    Wilner, David J.; Andrews, Sean M.; MacGregor, Meredith A. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Meredith Hughes, A. [Department of Astronomy, 601 Campbell Hall, University of California, Berkeley, CA 94720 (United States)

    2012-04-20

    We present imaging observations at 1.3 mm of the debris disk surrounding the nearby M-type flare star AU Mic with beam size 3'' (30 AU) from the Submillimeter Array. These data reveal a belt of thermal dust emission surrounding the star with the same edge-on geometry as the more extended scattered light disk detected at optical wavelengths. Simple modeling indicates a central radius of {approx}35 AU for the emission belt. This location is consistent with the reservoir of planetesimals previously invoked to explain the shape of the scattered light surface brightness profile through size-dependent dust dynamics. The identification of this belt further strengthens the kinship between the debris disks around AU Mic and its more massive sister star {beta} Pic, members of the same {approx}10 Myr old moving group.

  4. Growth of asteroids, planetary embryos and Kuiper belt objects by chondrule accretion

    E-Print Network [OSTI]

    Johansen, Anders; Lacerda, Pedro; Bizzarro, Martin

    2015-01-01

    Chondrules are millimeter-sized spherules that dominate primitive meteorites (chondrites) originating from the asteroid belt. The incorporation of chondrules into asteroidal bodies must be an important step in planet formation, but the mechanism is not understood. We show that the main growth of asteroids can result from gas-drag-assisted accretion of chondrules. The largest planetesimals of a population with a characteristic radius of 100 km undergo run-away accretion of chondrules within ~3 Myr, forming planetary embryos up to Mars sizes along with smaller asteroids whose size distribution matches that of main belt asteroids. The aerodynamical accretion leads to size-sorting of chondrules consistent with chondrites. Accretion of mm-sized chondrules and ice particles drives the growth of planetesimals beyond the ice line as well, but the growth time increases above the disk life time outside of 25 AU. The contribution of direct planetesimal accretion to the growth of both asteroids and Kuiper belt objects is...

  5. KUIPER BELT OBJECT OCCULTATIONS: EXPECTED RATES, FALSE POSITIVES, AND SURVEY DESIGN

    SciTech Connect (OSTI)

    Bickerton, S. J. [Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 (United States); Welch, D. L. [Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1 (Canada); Kavelaars, J. J. [Herzberg Institute of Astrophysics, Victoria, BC V9E 2E7 (Canada)], E-mail: bick@astro.princeton.edu, E-mail: welch@physics.mcmaster.ca, E-mail: JJ.Kavelaars@nrc-cnrc.gc.ca

    2009-05-15

    A novel method of generating artificial scintillation noise is developed and used to evaluate occultation rates and false positive rates for surveys probing the Kuiper Belt with the method of serendipitous stellar occultations. A thorough examination of survey design shows that (1) diffraction-dominated occultations are critically (Nyquist) sampled at a rate of 2 Fsu{sup -1}, corresponding to 40 s{sup -1} for objects at 40 AU, (2) occultation detection rates are maximized when targets are observed at solar opposition, (3) Main Belt asteroids will produce occultations light curves identical to those of Kuiper Belt Objects (KBOs) if target stars are observed at solar elongations of: 116{sup 0} {approx}< {epsilon} {approx}< 125 deg., or 131 deg. {approx}< {epsilon} {approx}< 141 deg., and (4) genuine KBO occultations are likely to be so rare that a detection threshold of {approx}>7-8{sigma} should be adopted to ensure that viable candidate events can be disentangled from false positives.

  6. STIS CORONAGRAPHIC IMAGING OF FOMALHAUT: MAIN BELT STRUCTURE AND THE ORBIT OF FOMALHAUT b

    SciTech Connect (OSTI)

    Kalas, Paul; Graham, James R. [Astronomy Department, University of California, Berkeley, CA 94720 (United States); Fitzgerald, Michael P. [Department of Physics and Astronomy, UCLA, Los Angeles, CA (United States); Clampin, Mark [NASA Goddard Space Flight Center, Greenbelt, MD (United States)

    2013-09-20

    We present new optical coronagraphic data of Fomalhaut obtained with HST/STIS in 2010 and 2012. Fomalhaut b is recovered at both epochs to high significance. The observations include the discoveries of tenuous nebulosity beyond the main dust belt detected to at least 209 AU projected radius, and a ?50 AU wide azimuthal gap in the belt northward of Fomalhaut b. The two epochs of Space Telescope Imaging Spectrograph (STIS) photometry exclude optical variability greater than 35%. A Markov chain Monte Carlo analysis demonstrates that the orbit of Fomalhaut b is highly eccentric, with e = 0.8 ± 0.1, a = 177 ± 68 AU, and q = 32 ± 24 AU. Fomalhaut b is apsidally aligned with the belt and 90% of allowed orbits have mutual inclination ?36°. Fomalhaut b's orbit is belt crossing in the sky plane projection, but only 12% of possible orbits have ascending or descending nodes within a 25 AU wide belt annulus. The high eccentricity invokes a dynamical history where Fomalhaut b may have experienced a significant dynamical interaction with a hypothetical planet Fomalhaut c, and the current orbital configuration may be relatively short-lived. The Tisserand parameter with respect to a hypothetical Fomalhaut planet at 30 AU or 120 AU lies in the range 2-3, similar to highly eccentric dwarf planets in our solar system. We argue that Fomalhaut b's minimum mass is that of a dwarf planet in order for a circumplanetary satellite system to remain bound to a sufficient radius from the planet to be consistent with the dust scattered light hypothesis. In the coplanar case, Fomalhaut b will collide with the main belt around 2032, and the subsequent emergent phenomena may help determine its physical nature.

  7. Louisiana Tech University Six Sigma Green Belt Certification A Louisiana Tech University Six Sigma Greenbelt certification can be obtained by

    E-Print Network [OSTI]

    Selmic, Sandra

    Louisiana Tech University Six Sigma Green Belt Certification A Louisiana Tech University Six Sigma Sigma and ENGR 566 Six Sigma and Quality Control with a B or higher. The cost to take the two required courses is $1,180 per course for a total of $2,360 to complete the Six Sigma Green Belt certification

  8. Radio-Loud and Radio-Quiet Gamma-Ray Pulsars from the Galactic Plane and the Gould Belt

    SciTech Connect (OSTI)

    Gonthier, P. L.

    2005-03-17

    We present recent results of a pulsar population synthesis study in the polar cap model that includes the Parkes Multibeam Pulsar Survey, realistic beam geometries for radio and {gamma}-ray emission from neutron stars born in the Galactic disc as well as the local Gould Belt. We include nine radio surveys to normalize the simulated results from the Galactic disc to the number of radio pulsars observed by the group of selected surveys. In normalizing the contribution of the Gould Belt, we use results from a recent study that indicates a supernova rate in the Gould Belt of 3 to 5 times that of the local region of the Galactic plane leading to {approx}100 neutron stars born in the Gould Belt during the last 5 Myr. Our simulations include the dynamical evolution of the Gould Belt where neutron stars are produced in the plane of the Gould Belt during the past 5 Myr. We discuss the simulated numbers of radio-quiet (those below flux threshold of radio surveys) and radio-loud, {gamma}-ray pulsars from the Galactic disc and the Gould belt observed by {gamma}-ray telescopes EGRET, AGILE and GLAST. They suggest that about 35 of the unidentified EGRET sources could be (mostly radio-loud) {gamma}-ray pulsars with 2/3 of them born in the Galactic disc and 1/3 in the Gould Belt.

  9. Steady-State Impurity Control, Heat Removal and Tritium Recovery by Moving-Belt Plasma-Facing Components

    E-Print Network [OSTI]

    Tillack, Mark

    1 Steady-State Impurity Control, Heat Removal and Tritium Recovery by Moving-Belt Plasma-Z getter materials, heat removal and tritium recovery. In order to minimize MHD effects as well as induced is the application of "Moving-Belt Plasma-Facing Components" for steady-state impurity gettering, heat removal

  10. The Evidence for Slow Migration of Neptune from the Inclination Distribution of Kuiper Belt Objects

    E-Print Network [OSTI]

    Nesvorny, David

    2015-01-01

    Much of the dynamical structure of the Kuiper belt can be explained if Neptune migrated over several AU, and/or if Neptune was scattered to an eccentric orbit during planetary instability. An outstanding problem with the existing formation models is that the distribution of orbital inclinations they predicted is narrower than the one inferred from observations. Here we perform numerical simulations of Kuiper belt formation starting from an initial state with Neptune at 20 = 10 Myr and a_{N,0} 40 AU region, where the Cold Classicals presumably formed.

  11. MILLIMETER IMAGING OF THE {beta} PICTORIS DEBRIS DISK: EVIDENCE FOR A PLANETESIMAL BELT

    SciTech Connect (OSTI)

    Wilner, David J.; Andrews, Sean M. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Hughes, A. Meredith [Department of Astronomy, 601 Campbell Hall, University of California, Berkeley, CA 94720 (United States)

    2011-02-01

    We present observations at 1.3 mm wavelength of the {beta} Pictoris debris disk with beam size 4.''3 x 2.''6 (83 x 50 AU) from the Submillimeter Array. The emission shows two peaks separated by {approx}7'' along the disk plane, which we interpret as a highly inclined dust ring or belt. A simple model constrains the belt center to 94 {+-} 8 AU, close to the prominent break in slope of the optical scattered light. We identify this region as the location of the main reservoir of dust-producing planetesimals in the disk.

  12. Geology of a portion of the northern Kings Mountain belt, North Carolina 

    E-Print Network [OSTI]

    Michie, Joanna

    1985-01-01

    GEOLOGY OF A PORTrON OP THE NORTHERN RINGS YOUNTAIN BELT NO&TH CAROLINA A Thesis by JOANNA NICHIF Submitted to the Graduate College of Texas A&M University in partial fulfillment of the requirements for the degree of MASTER OF SCIENCE Hay... lep5 Yaior Subiect: Geology GEOLOGY OF A PORTION OF THE NORTHERN KINGS MOUNTAIN BELT, NORTH CAROLINA A Thesis by JOANNA MICHIE Approved as to style and content by: David W. Mohr (Chairman of Committee) J. Robert Butler (Member) John H. pang...

  13. GEOPHYSICAL RESEARCH LETTERS, VOL. 0, NO. 0, PAGES 0-0, M 0, 2001 Long Term Measurements of Radiation Belts by

    E-Print Network [OSTI]

    Li, Xinlin

    of Radiation Belts by SAMPEX and Their Variations Xinlin Li,1 D. N. Baker,1 S. G. Kanekal,1 M. Looper,2 M-altitude and polar- orbiting satellite, has provided a long-term global picture of the radiation belts since its launch on July 3, 1992. While the inner belt (L

  14. The Antarctic Circumpolar Productivity Belt Joint Institute for the Study of the Atmosphere and Ocean, University of Washington, Seattle, Washington, USA

    E-Print Network [OSTI]

    Follows, Mick

    The Antarctic Circumpolar Productivity Belt T. Ito Joint Institute for the Study of the Atmosphere in the Southern Ocean using a coupled, physical-biogeochemical-ecological model. The model captures a belt of enhanced export production, figuratively termed as the Antarctic Circumpolar Productivity Belt. As observed

  15. JOURNAL OF GEOPHYSICAL RESEARCH: SOLID EARTH, VOL. 118, 120, doi:10.1002/jgrb.50258, 2013 Lithospheric structure of an Archean craton and adjacent mobile belt

    E-Print Network [OSTI]

    Jones, Alan G.

    Lithospheric structure of an Archean craton and adjacent mobile belt revealed from 2-D and 3-D inversion; accepted 20 June 2013. [1] Archean cratons, and the stitching Proterozoic orogenic belts on their flanks-African orogenic belt due to thick sedimentary cover. We present the first lithospheric-scale geophysical study

  16. THE OUTER EDGE OF THE KUIPER BELT. J. M. Hahn, Lunar and Planetary Institute, Houston TX 77058, USA, (hahn@lpi.usra.edu).

    E-Print Network [OSTI]

    Hahn, Joseph M.

    THE OUTER EDGE OF THE KUIPER BELT. J. M. Hahn, Lunar and Planetary Institute, Houston TX 77058, USA, (hahn@lpi.usra.edu). One of the more curious features of the Kuiper Belt is the apparent dearth of Kuiper Belt Objects (KBOs) orbiting the Sun beyond 50 AU with modest eccentricities and incli- nations, e

  17. Journal of the Geological Society, London, Vol. 160, 2003, pp. 677685. Printed in Great Britain. Tectonic evolution of the NE Palmyride mountain belt, Syria

    E-Print Network [OSTI]

    . 677 Tectonic evolution of the NE Palmyride mountain belt, Syria: the Bishri crustal block GRAHAM BREW1 is a broad NE-plunging inverted basin located at the NE portion of the Palmyride mountain belt where that has driven the evolution of intracontinental Syria. Keywords: Palmyride mountain belt, Syria, seismic

  18. JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 97, NO. BIO, PAGES 14,207-14,221, SEPTEMBER lO, 1992 On the Stability of Isostatically Compensated Mountain Belts

    E-Print Network [OSTI]

    Sandiford, Mike

    On the Stability of Isostatically Compensated Mountain Belts SHAOHUA ZHOU AND MICHAEL SANDIFORD Department of convergent mountain belts is invariably accompanied by an increase in grav- itational potential energy due of isostatically compensated mountain belts under the assumption that the strength of continental Iithosphere

  19. EXTREME KUIPER BELT OBJECT 2001 QG298 AND THE FRACTION OF CONTACT BINARIES Scott S. Sheppard and David C. Jewitt1

    E-Print Network [OSTI]

    Jewitt, David C.

    EXTREME KUIPER BELT OBJECT 2001 QG298 AND THE FRACTION OF CONTACT BINARIES Scott S. Sheppard ABSTRACT Extensive time-resolved observations of Kuiper belt object 2001 QG298 show a light curve of 0.04 (0.10) is assumed. This is the first known Kuiper belt object and only the third minor planet

  20. UPb Silurian age for a gabbro of the Platinum-bearing Belt of the Middle Urals (Russia): evidence for beginning of closure of the Uralian Ocean

    E-Print Network [OSTI]

    Demouchy, Sylvie

    U­Pb Silurian age for a gabbro of the Platinum-bearing Belt of the Middle Urals (Russia): evidence-bearing Belt of the Urals consists of a series of zoned ultramafic bodies obducted onto the passive continental that the Uralian Platinum-bearing Belt is best interpreted as remnants of an island-arc oceanic lithosphere

  1. Abstract, 2011 Advances in Earth Science Research Conference 2011 Petrogenesis of the Metavolcanic Rocks of the North Caribou Greenstone Belt: Implications for

    E-Print Network [OSTI]

    Rocks of the North Caribou Greenstone Belt: Implications for tectonic evolution of the Archean greenstone belt J. Duff1 , K. Hattori1 and D.A. Schneider1 1 Department of Earth Sciences, University with the presence of 3.0 Ga quartz arenite and a 3.45 Ga zircon. The North Caribou belt, approximately 10 km

  2. Source and tectono-metamorphic evolution of mafic and pelitic metasedimentary rocks from the central Quetico metasedimentary belt, Archean Superior Province

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    the central Quetico metasedimentary belt, Archean Superior Province of Canada Franck Vallia* , Stephane Abstract A study of the Jean Lake area of the Quetico metasedimentary belt, Superior Province, Canada to the Wabigoon subprovince to the north and Wawa greenstone belt to the south. The P-T-time path of this Archean

  3. ApJ, in press November 3, 2013 The density of mid-sized Kuiper belt object 2002 UX25 and the

    E-Print Network [OSTI]

    Brown, Michael E.

    ApJ, in press November 3, 2013 The density of mid-sized Kuiper belt object 2002 UX25 in the Kuiper belt, with measured den- sities of 1.5 g cm-3 and higher, from the coagulation of small bodies for diameters larger than 350 km. In the Kuiper belt, no density measurements have been made between 350 km

  4. Early Paleozoic tectonic evolution of the Xing-Meng Orogenic Belt: constraints from detrital zircon geochronology of western Erguna-Xing'an Block, North China

    E-Print Network [OSTI]

    Boyer, Edmond

    Early Paleozoic tectonic evolution of the Xing-Meng Orogenic Belt: constraints from detrital zircon,c,d , Faure Michelb,c,d a Key Laboratory of Orogenic Belts and Crustal Evolution, Ministry of Education is similar to those from adjacent blocks in the southeastern Central Asian Orogenic Belt. Taking previous

  5. THE SECULAR EVOLUTION OF THE PRIMORDIAL KUIPER BELT. J. M. Hahn, Lunar and Planetary Institute, Houston TX 77058, USA, (hahn@lpi.usra.edu).

    E-Print Network [OSTI]

    Hahn, Joseph M.

    THE SECULAR EVOLUTION OF THE PRIMORDIAL KUIPER BELT. J. M. Hahn, Lunar and Planetary Institute, Houston TX 77058, USA, (hahn@lpi.usra.edu). The Kuiper Belt is a vast swarm of comets orbiting at the Solar System's outer edge. This Belt is comprised of debris that was left over from the epoch of planet

  6. Reanalysis of Radiation Belt Electron Phase Space Density using the UCLA 1-D VERB code and Kalman filtering: Sensitivity to assumed

    E-Print Network [OSTI]

    Ghil, Michael

    Reanalysis of Radiation Belt Electron Phase Space Density using the UCLA 1-D VERB code and Kalman of improving current radiation belt models and achieving predictive capabilities. In the future data of radiation belt electron phase space density using the VERB code and a Kalman filter to the assumed location

  7. EXPORT CONTROLS PREPARED BY

    E-Print Network [OSTI]

    Sorin, Eric J.

    EXPORT CONTROLS MANUAL PREPARED BY: Office of General Counsel The California State University SEPTEMBER 2012 #12; Export Controls Manual Table of Contents I. INTRODUCTION ......................................................................................................... 1 II. HISTORY OF EXPORT CONTROLS

  8. Analysis of Heavy Oil Recovery by Thermal EOR in a Meander Belt: From Geological

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    Analysis of Heavy Oil Recovery by Thermal EOR in a Meander Belt: From Geological to Reservoir- zation of fluvial meandering reservoirs and petrophysical properties are required for uncertainty Modeling R. Deschamps*, N. Guy, C. Preux and O. Lerat 1 IFP Energies nouvelles, 1-4 avenue de Bois

  9. Quantification of the precipitation loss of radiation belt electrons observed by SAMPEX

    E-Print Network [OSTI]

    Li, Xinlin

    Click Here for Full Article Quantification of the precipitation loss of radiation belt electrons/PET observations, the rates and the spatial and temporal variations of electron loss to the atmosphere in the Earth and pitch angle diffusion. The measured electrons by SAMPEX can be distinguished as trapped, quasi trapped

  10. A nonstorm time enhancement of relativistic electrons in the outer radiation belt

    E-Print Network [OSTI]

    Li, Xinlin

    A nonstorm time enhancement of relativistic electrons in the outer radiation belt Quintin Schiller (based on the Dst index), relativistic electron fluxes were enhanced over 2.5 orders of magnitude Electron Ion Spectrometer (MagEIS), onboard the Van Allen Probes; Relativistic Electron and Proton

  11. Pitch angle distribution analysis of radiation belt electrons based on Combined Release and Radiation Effects Satellite

    E-Print Network [OSTI]

    Li, Xinlin

    Pitch angle distribution analysis of radiation belt electrons based on Combined Release and Radiation Effects Satellite Medium Electrons A data J. L. Gannon,1 X. Li,1 and D. Heynderickx2 Received 13 the Medium Electrons A instrument on the Combined Release and Radiation Effects Satellite (CRRES), a survey

  12. Analysis of radiation belt energetic electron phase space density using THEMIS SST measurements: Crosssatellite calibration

    E-Print Network [OSTI]

    California at Berkeley, University of

    Laboratory (LANL) satellite LANL01A synchronous orbit particle analyzer (SOPA) for a half year period SOPA instrument, the THEMIS SST underestimates the electron fluxes within a factor of 2 for the 40 and the SOPA measurements from the LANL01A and 1989­048 satellites, we analyze the response of radiation belt

  13. Terrestrial Planet Formation Constrained by Mars and the Structure of the Asteroid Belt

    E-Print Network [OSTI]

    Izidoro, André; Morbidelli, Alessandro; Winter, Othon C

    2015-01-01

    Reproducing the large Earth/Mars mass ratio requires a strong mass depletion in solids within the protoplanetary disk between 1 and 3 AU. The Grand Tack model invokes a specific migration history of the giant planets to remove most of the mass initially beyond 1 AU and to dynamically excite the asteroid belt. However, one could also invoke a steep density gradient created by inward drift and pile-up of small particles induced by gas-drag, as has been proposed to explain the formation of close-in super Earths. Here we show that the asteroid belt's orbital excitation provides a crucial constraint against this scenario for the Solar System. We performed a series of simulations of terrestrial planet formation and asteroid belt evolution starting from disks of planetesimals and planetary embryos with various radial density gradients and including Jupiter and Saturn on nearly circular and coplanar orbits. Disks with shallow density gradients reproduce the dynamical excitation of the asteroid belt by gravitational s...

  14. A spectroscopic comparison of HED meteorites and V-type asteroids in the inner Main Belt

    E-Print Network [OSTI]

    Moskovitz, Nicholas A.

    V-type asteroids in the inner Main Belt (a < 2.5 AU) and the HED meteorites are thought to be genetically related to one another as collisional fragments from the surface of the large basaltic Asteroid 4 Vesta. We investigate ...

  15. The Kuiper Belt Luminosity Function from m(R)=21 to 26

    E-Print Network [OSTI]

    W. C. Fraser; JJ Kavelaars; M. J. Holman; C. J. Pritchet; B. J Gladman; T. Grav; R. L. Jones; J. MacWilliams; J. -M. Petit

    2008-02-17

    We have performed an ecliptic imaging survey of the Kuiper belt with our deepest and widest field achieving a limiting flux of m(g') = 26.4, with a sky coverage of 3.0 square-degrees. This is the largest coverage of any other Kuiper belt survey to this depth. We detect 72 objects, two of which have been previously observed. We have improved the Bayesian maximum likelihood fitting technique presented in Gladman et al. (1998) to account for calibration and sky density variations and have used this to determine the luminosity function of the Kuiper belt. Combining our detections with previous surveys, we find the luminosity function is well represented by a single power-law with slope alpha = 0.65 +/- 0.05 and an on ecliptic sky density of 1 object per square-degree brighter than m(R)=23.42 +/- 0.13. Assuming constant albedos, this slope suggests a differential size-distribution slope of 4.25 +/- 0.25, which is steeper than the Dohnanyi slope of 3.5 expected if the belt is in a state of collisional equilibrium. We find no evidence for a roll-over or knee in the luminosity function and reject such models brightward of m(R) ~ 24.6.

  16. School Name Team Name Coach/Teacher Bloomfield HS Van Allen Belts Jason McCaughey

    E-Print Network [OSTI]

    Devoret, Michel H.

    School Name Team Name Coach/Teacher Bloomfield HS Van Allen Belts Jason Mc Rangers Peter Schmitt Mauro Sheridan Middle School Apple Sue Brown Mercy HS Quanta Buff Bachenheimer Millbrook School Spooky Action Somerset Waters Naugatuck HS Gone Fission Marc Pardee

  17. Adaptive Linear Prediction of Radiation Belt Electrons Using the Kalman Filter

    E-Print Network [OSTI]

    to changes in solar wind bulk speed using linear prediction filters [Baker et al., 1990; Vassiliadis et alAdaptive Linear Prediction of Radiation Belt Electrons Using the Kalman Filter E.J. Rigler, D improvement in zero-time-lag electron log-flux "predictions" relative to models that are based on time

  18. Method for determining molten metal pool level in twin-belt continuous casting machines

    DOE Patents [OSTI]

    Kaiser, Timothy D. (Colchester, VT); Daniel, Sabah S. (Pittsburgh, PA); Dykes, Charles D. (Milton, VT)

    1989-03-21

    A method for determining level of molten metal in the input of a continuous metal casting machine having at least one endless, flexible, revolving casting belt with a surface which engages the molten metal to be cast and a reverse, cooled surface along which is directed high velocity liquid coolant includes the steps of predetermining the desired range of positions of the molten metal pool and positioning at least seven heat-sensing transducers in bearing contact with the moving reverse belt surface and spaced in upstream-downstream relationship relative to belt travel spanning the desired pool levels. A predetermined temperature threshold is set, somewhat above coolant temperature and the output signals of the transducer sensors are scanned regarding their output signals indicative of temperatures of the moving reverse belt surface. Position of the molten pool is determined using temperature interpolation between any successive pair of upstream-downstream spaced sensors, which follows confirmation that two succeeding downstream sensors are at temperature levels exceeding threshold temperature. The method accordingly provides high resolution for determining pool position, and verifies the determined position by utilizing full-strength signals from two succeeding downstream sensors. In addition, dual sensors are used at each position spanning the desired range of molten metal pool levels to provide redundancy, wherein only the higher temperature of each pair of sensors at a station is utilized.

  19. GEOSPATIAL DECISION SUPPORT FOR SEED COMPANIES IN THE CORN BELT Marcus E. Tooze1

    E-Print Network [OSTI]

    Reichenbach, Stephen E.

    agroecological regions where Golden Harvest's suite of corn hybrids were bested adapted in the western Corn Belt qualities and root zone water-holding capacities, reducing risks to drought events. A toolkit of ESRI Arc Harvest brand products, outlined a series of issues within their business model to improve acreage

  20. METHANE AND ETHANE ON THE BRIGHT KUIPER BELT OBJECT 2005 FY9 M. E. Brown,1

    E-Print Network [OSTI]

    Brown, Michael E.

    METHANE AND ETHANE ON THE BRIGHT KUIPER BELT OBJECT 2005 FY9 M. E. Brown,1 K. M. Barkume,1 G. A indicates the clear presence of ethane, an expected product of UV photolysis of methane. No evidence for N2 of 2005 FY9 that leads to large methane grains, abundant sites for ethane formation through UV photolysis

  1. Frontline Earth Science Research @ St Andrews The Rise and Fall of Mountain Belts

    E-Print Network [OSTI]

    Brierley, Andrew

    1 Frontline Earth Science Research @ St Andrews (FRESH) The Rise and Fall of Mountain Belts 18 and for controlling the tectonics of mountain building by Z ZZ- dZ ZZ tween tectonics and anatexis and establish (28-23 Ma) suite comprises anastamosing sheets of foli- ated two-mica, garnet-bearing granite

  2. Variations in ground surface temperature histories in the Thompson Belt, Manitoba, Canada: environment and climate changes

    E-Print Network [OSTI]

    Long, Bernard

    history (GSTH) obtained by the inversion of Pipe Mine temperature profiles suggests that a recent (50Variations in ground surface temperature histories in the Thompson Belt, Manitoba, Canada recherche en ge´ochimie et ge´odynamique, Universite´ du Que´bec a` Montre´al, C.P. 8888, succ. ``Centre

  3. Deformation regime variations in an arcuate transpressional orogen (Ribeira belt, SE Brazil) imaged by anisotropy of

    E-Print Network [OSTI]

    Bascou, Jérôme

    Deformation regime variations in an arcuate transpressional orogen (Ribeira belt, SE Brazil) imaged Paulo, Brazil b Laboratoire de Tectonophysique, Universite´ de Montpellier II CNRS, Montpellier, France Instituto de Geocie^ncias, Universidade Federal de Minas Gerais, Minas Gerais, Brazil Received 23 September

  4. Seismic imaging of the lithospheric structure of the Zagros mountain belt (Iran)

    E-Print Network [OSTI]

    Hatzfeld, Denis

    Seismic imaging of the lithospheric structure of the Zagros mountain belt (Iran) ANNE PAUL1*, DENIS International Institute of Earthquake Engineering and Seismology, Tehran, Iran 3 Institute for Advanced Studies in Basic Sciences (IASBS), PO Box 45195-1159, Zanjan, Iran *Corresponding author (e-mail: Anne

  5. AN ASTEROID BELT INTERPRETATION FOR THE TIMING VARIATIONS OF THE MILLISECOND PULSAR B1937+21

    SciTech Connect (OSTI)

    Shannon, R. M.; Cordes, J. M. [Astronomy Department, Cornell University, Ithaca, NY 14853 (United States)] [Astronomy Department, Cornell University, Ithaca, NY 14853 (United States); Metcalfe, T. S. [Space Science Institute, 4750 Walnut Street Suite 205, Boulder, CO 80301 (United States)] [Space Science Institute, 4750 Walnut Street Suite 205, Boulder, CO 80301 (United States); Lazio, T. J. W. [Jet Propulsion Laboratory, California Institute of Technology, M/S 138-308, Pasadena, CA 91109 (United States)] [Jet Propulsion Laboratory, California Institute of Technology, M/S 138-308, Pasadena, CA 91109 (United States); Cognard, I.; Desvignes, G.; Theureau, G. [LPC2E/CNRS-Universite d'Orleans, Orleans, F-45071, Cedex 2 (France)] [LPC2E/CNRS-Universite d'Orleans, Orleans, F-45071, Cedex 2 (France); Janssen, G. H.; Purver, M. B.; Stappers, B. W. [University of Manchester and Jodrell Bank Observatory, Manchester, M13 9PL (United Kingdom)] [University of Manchester and Jodrell Bank Observatory, Manchester, M13 9PL (United Kingdom); Jessner, A.; Kramer, M.; Lazaridis, K., E-mail: ryan.shannon@csiro.au, E-mail: cordes@astro.cornell.edu [Max-Planck-Institut fuer Radioastonomie, Bonn, D-53121 (Germany)

    2013-03-20

    Pulsar timing observations have revealed companions to neutron stars that include other neutron stars, white dwarfs, main-sequence stars, and planets. We demonstrate that the correlated and apparently stochastic residual times of arrival from the millisecond pulsar B1937+21 are consistent with the signature of an asteroid belt having a total mass {approx}< 0.05 M{sub Circled-Plus }. Unlike the solar system's asteroid belt, the best fit pulsar asteroid belt extends over a wide range of radii, consistent with the absence of any shepherding companions. We suggest that any pulsar that has undergone accretion-driven spin-up and subsequently evaporated its companion may harbor orbiting asteroid mass objects. The resulting timing variations may fundamentally limit the timing precision of some of the other millisecond pulsars. Observational tests of the asteroid belt model include identifying periodicities from individual asteroids, which are difficult; testing for statistical stationarity, which becomes possible when observations are conducted over a longer observing span; and searching for reflected radio emission.

  6. NEPTUNE ON TIPTOES: DYNAMICAL HISTORIES THAT PRESERVE THE COLD CLASSICAL KUIPER BELT

    SciTech Connect (OSTI)

    Wolff, Schuyler [Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218 (United States); Dawson, Rebekah I.; Murray-Clay, Ruth A., E-mail: swolff@pha.jhu.edu, E-mail: rdawson@cfa.harvard.edu, E-mail: rmurray-clay@cfa.harvard.edu [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)

    2012-02-20

    The current dynamical structure of the Kuiper Belt was shaped by the orbital evolution of the giant planets, especially Neptune, during the era following planet formation when the giant planets may have undergone planet-planet scattering and/or planetesimal-driven migration. Numerical simulations of this process, while reproducing many properties of the Belt, fail to generate the high inclinations and eccentricities observed for some objects while maintaining the observed dynamically 'cold' population. We present the first of a three-part parameter study of how different dynamical histories of Neptune sculpt the planetesimal disk. Here we identify which dynamical histories allow an in situ planetesimal disk to remain dynamically cold, becoming today's cold Kuiper Belt population. We find that if Neptune undergoes a period of elevated eccentricity and/or inclination, it secularly excites the eccentricities and inclinations of the planetesimal disk. We demonstrate that there are several well-defined regimes for this secular excitation, depending on the relative timescales of Neptune's migration, the damping of Neptune's orbital inclination and/or eccentricity, and the secular evolution of the planetesimals. We model this secular excitation analytically in each regime, allowing for a thorough exploration of parameter space. Neptune's eccentricity and inclination can remain high for a limited amount of time without disrupting the cold classical belt. In the regime of slow damping and slow migration, if Neptune is located (for example) at 20 AU, then its eccentricity must stay below 0.18 and its inclination below 6 Degree-Sign .

  7. An Outer Planet Beyond Pluto and Origin of the Trans-Neptunian Belt Architecture

    E-Print Network [OSTI]

    Patryk Sofia Lykawka; Tadashi Mukai

    2007-12-13

    Trans-Neptunian objects (TNOs) are remnants of a collisionally and dynamically evolved planetesimal disk in the outer solar system. This complex structure, known as the trans-Neptunian belt (or Edgeworth-Kuiper belt), can reveal important clues about disk properties, planet formation, and other evolutionary processes. In contrast to the predictions of accretion theory, TNOs exhibit surprisingly large eccentricities, e, and inclinations, i, which can be grouped into distinct dynamical classes. Several models have addressed the origin and orbital evolution of TNOs, but none have reproduced detailed observations, e.g., all dynamical classes and peculiar objects, or provided insightful predictions. Based on extensive simulations of planetesimal disks with the presence of the four giant planets and massive planetesimals, we propose that the orbital history of an outer planet with tenths of Earth's mass can explain the trans-Neptunian belt orbital structure. This massive body was likely scattered by one of the giant planets, which then stirred the primordial planetesimal disk to the levels observed at 40-50 AU and truncated it at about 48 AU before planet migration. The outer planet later acquired an inclined stable orbit (>100 AU; 20-40 deg) because of a resonant interaction with Neptune (an r:1 or r:2 resonance possibly coupled with the Kozai mechanism), guaranteeing the stability of the trans-Neptunian belt. Our model consistently reproduces the main features of each dynamical class with unprecedented detail; it also satisfies other constraints such as the current small total mass of the trans-Neptunian belt and Neptune's current orbit at 30.1 AU. We also provide observationally testable predictions.

  8. Evidence for a colour dependence in the size distribution of main belt asteroids

    E-Print Network [OSTI]

    Paul Wiegert; David Balam; Andrea Moss; Christian Veillet; Martin Connors; Ian Shelton

    2006-11-09

    We present the results of a project to detect small (~1 km) main-belt asteroids with the 3.6 meter Canada-France-Hawaii Telescope (CFHT). We observed in 2 filters (MegaPrime g' and r') in order to compare the results in each band. Owing to the observational cadence we did not observe the same asteroids through each filter and thus do not have true colour information. However strong differences in the size distributions as seen in the two filters point to a colour-dependence at these sizes, perhaps to be expected in this regime where asteroid cohesiveness begins to be dominated by physical strength and composition rather than by gravity. The best fit slopes of the cumulative size distributions (CSDs) in both filters tend towards lower values for smaller asteroids, consistent with the results of previous studies. In addition to this trend, the size distributions seen in the two filters are distinctly different, with steeper slopes in r' than in g'. Breaking our sample up according to semimajor axis, the difference between the filters in the inner belt is found to be somewhat less pronounced than in the middle and outer belt, but the CSD of those asteroids seen in the r' filter is consistently and significantly steeper than in g' throughout. The CSD slopes also show variations with semimajor axis within a given filter, particularly in r'. We conclude that the size distribution of main belt asteroids is likely to be colour dependent at kilometer sizes and that this dependence may vary across the belt.

  9. Study of movement of the western and central belts of Peninsular Malaysia using GPS data analysis

    SciTech Connect (OSTI)

    Ramli, Siti Hafizah; Samsudin, Abdul Rahim [Geology Programme, School of Environmental and Natural Resource Sciences, Faculty of Science and Technology, Universiti Kebangsaan Malaysia, 43600 Bangi, Selangor (Malaysia)

    2014-09-03

    Since the large earthquakes in Sumatera and Nias, there were some tremors incidents at Bukit Tinggi. Therefore, a study on the earth’s crust movement and the effects of the earthquake in Indonesia on the tectonic blocks of Peninsular Malaysia have been carried out using GPS data analysis. GPS data from five MyRTKnet stations within Peninsular Malaysia have been analyzed to monitor the movement of two major tectonic blocks of Peninsular Malaysia which are the western belt represented by the Behrang (BEHR) and UPM Serdang (UPMS) stations and the central belt represented by Bentong (BENT), Jerantut (JRNT) and Temerloh (TLOH) stations. GPS data recorded from 2005 to 2010 were analysed based on horizontal and vertical displacements of the respective stations by using Trimble Business Centre (TBC) software. Based on the results of accumulated displacements of recorded GPS data from January 2006 to December 2013, it shows that the western belt which represented by UPMS has shifted 0.096m towards northwest with changes of ellipsoidal height of +0.030m while the central belt which represented by TLOH has shifted 0.080m towards northwest with changes of ellipsoidal height of ?0.015m. Meanwhile, BENT station which is located on the Bentong-Raub suture zone turns to its original position as well as JRNT station. However, BEHR station which are located in western belt do not show any movements. All of these movements may be due to the influence of reactive faults in the stations area stimulated by several large earthquakes that occurred in 2005 to 2010. Study on using the GPS data analysis and combine with integrated geophysical methods are necessary to understand in detail about the tectonic evolution of Peninsular Malaysia.

  10. EVIDENCE FROM THE ASTEROID BELT FOR A VIOLENT PAST EVOLUTION OF JUPITER'S ORBIT

    SciTech Connect (OSTI)

    Morbidelli, Alessandro; Brasser, Ramon [Departement Cassiopee, Universite de Nice-Sophia Antipolis, Observatoire de la Cote d'Azur, CNRS 4, 06304 Nice (France); Gomes, Rodney [Observatrio Nacional, Rua General Jos Cristino 77, CEP 20921-400, Rio de Janeiro, RJ (Brazil); Levison, Harold F. [Southwest Research Institute, 1050 Walnut St., Suite 300, Boulder, CO 80302 (United States); Tsiganis, Kleomenis [Department of Physics, Aristotle University of Thessaloniki, 54 124 Thessaloniki (Greece)

    2010-11-15

    We use the current orbital structure of large (>50 km) asteroids in the main asteroid belt to constrain the evolution of the giant planets when they migrated from their primordial orbits to their current ones. Minton and Malhotra showed that the orbital distribution of large asteroids in the main belt can be reproduced by an exponentially decaying migration of the giant planets on a timescale of {tau} {approx} 0.5 Myr. However, self-consistent numerical simulations show that the planetesimal-driven migration of the giant planets is inconsistent with an exponential change in their semi-major axes on such a short timescale. In fact, the typical timescale is {tau} {>=} 5 Myr. When giant planet migration on this timescale is applied to the asteroid belt, the resulting orbital distribution is incompatible with the observed one. However, the planet migration can be significantly sped up by planet-planet encounters. Consider an evolution where both Jupiter and Saturn have close encounters with a Neptune-mass planet (presumably Uranus or Neptune itself) and where this third planet, after being scattered inward by Saturn, is scattered outward by Jupiter. This scenario leads to a very rapid increase in the orbital separation between Jupiter and Saturn which we show here to have only mild effects on the structure of the asteroid belt. This type of evolution is called a 'jumping-Jupiter' case. Our results suggest that the total mass and dynamical excitation of the asteroid belt before migration were comparable to those currently observed. Moreover, they imply that, before migration, the orbits of Jupiter and Saturn were much less eccentric than their current ones.

  11. Review: Preparing for Climate Change

    E-Print Network [OSTI]

    Kunnas, Jan

    2013-01-01

    Review: Preparing for Climate Change By Michael D.Stephen, Preparing for Climate Change. A Boston Review Book.alkaline paper. “Climate change is inevitable, but disaster

  12. INTERPRETING THE KUIPER BELT LUMINOSITY FUNCTION. J. M. Hahn, Lunar and Planetary Institute, Houston TX 77058-1113, USA,(hahn@lpi.jsc.nasa.gov), L. Brown, ColgateUniversity, HamiltonNY 13346, USA,(labrown@center.colgate.edu).

    E-Print Network [OSTI]

    Hahn, Joseph M.

    INTERPRETING THE KUIPER BELT LUMINOSITY FUNCTION. J. M. Hahn, Lunar and Planetary Institute,(labrown@center.colgate.edu). The Kuiper Belt luminosity function m, which is the number density of Kuiper Belt Objects (KBOs) observable that increases with distance. Although most treatments of the Kuiper Belt assume a primordial radial distribution

  13. Dynamical determination of the Kuiper Belt's mass from motions of the inner planets of the Solar System

    E-Print Network [OSTI]

    Lorenzo Iorio

    2006-11-08

    In this paper we dynamically determine the mass of the Kuiper Belt Objects by exploiting the latest observational determinations of the orbital motions of the inner planets of the Solar System. Our result, in units of terrestrial masses, is 0.033 +/- 0.115 by modelling the Classical Kuiper Belt Objects as an ecliptic ring of finite thickness. A two-rings model yields for the Resonant Kuiper Belt Objects a value of 0.018 +/- 0.063. Such figures are consistent with recent determinations obtained with ground and space-based optical techniques. Some implications for precise tests of Einsteinian and post-Einsteinian gravity are briefly discussed.

  14. Participants were asked to generate aloud either the object's common use (e.g., belt: to keep one's pants up) or an uncommon use for it (e.g., belt: to use as a tourniquet). Participants received the Forward Digit Span

    E-Print Network [OSTI]

    Thompson-Schill, Sharon

    Procedure Participants were asked to generate aloud either the object's common use (e.g., belt: to keep one's pants up) or an uncommon use for it (e.g., belt: to use as a tourniquet). Participants

  15. A survey of ideal fluid propeller theories and a study of the effects of aerodynamic propeller loading on trailing vortex induced velocity and thrust 

    E-Print Network [OSTI]

    Kelley, Edward Madison

    1969-01-01

    A SURVEY OF IDEAL FLUID PRO~ THEORIES AND A STUIE OP THE EFFECTS OF AERODYNAMIC PRO~ LOADING ON TRAILING VORTEX INDUCED VELOCITY AND THRUST A Thesis EDWARD MADISON ~ Suhmitted to the Graduate College of Texas A&M University in Partial... VELOCITY AND THRUST A Thesis by EDWARD MADISON HELLEY Approsed as to sty1e and content 'by: Head of epartment i%. mbe August 1969 111 ABSTRACT A Survey of Ideal Fluid Propeller Theories and a Study of the Ei'fects of Aerodynamic Propeller...

  16. HERSCHEL-RESOLVED OUTER BELTS OF TWO-BELT DEBRIS DISKS AROUND A-TYPE STARS: HD 70313, HD 71722, HD 159492, AND F-TYPE: HD 104860

    SciTech Connect (OSTI)

    Morales, F. Y.; Bryden, G.; Werner, M. W. [Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109 (United States); Stapelfeldt, K. R., E-mail: Farisa@jpl.nasa.gov [NASA Goddard Space Flight Center, Exoplanets and Stellar Astrophysics Laboratory, Code 667, Greenbelt, MD 20771 (United States)

    2013-10-20

    We present dual-band Herschel/Photodetector Array Camera and Spectrometer imaging for four stars whose spectral energy distributions (SEDs) suggest two-ring disk architectures that mirror that of the asteroid-Kuiper Belt geometry of our own solar system. The Herschel observations at 100 ?m spatially resolve the cold/outer-dust component for each star-disk system for the first time, finding evidence of planetesimals at >100 AU, i.e., a larger size than assumed from a simple blackbody fit to the SED. By breaking the degeneracy between the grain properties and the dust's radial location, the resolved images help constrain the dust grain-size distribution for each system. Three of the observed stars are A-type and one solar-type. On the basis of the combined Spitzer/IRS+MIPS (5-70 ?m), the Herschel/PACS (100 and 160 ?m) dataset, and under the assumption of idealized spherical grains, we find that the cold/outer belts of the three A-type stars are well fit with a mixed ice/rock composition rather than pure rocky grains, while the debris around the solar-type star is consistent with either rock or ice/rock grains. For the solar-type star HD 104860, we find that the minimum grain size is larger than expected from the threshold set by radiative blowout. The A-type stars HD 71722 and HD 159492, on the other hand, require minimum grain sizes that are smaller than blowout for inner- and outer-ring populations. In the absence of spectral features for ice, we find that the behavior of the continuum can help constrain the composition of the grains (of icy nature and not pure rocky material) given the Herschel-resolved locations of the cold/outer-dust belts.

  17. Preparation of ethylenediamine dinitrate

    DOE Patents [OSTI]

    Lee, K.

    1984-05-17

    Method for the preparation of ethylenediamine dinitrate. Ethylenediamine dinitrate, a useful explosive, may readily be prepared by solvent extraction of nitrate ion from an acidic aqueous solution thereof using a high-molecular-weight, water-insoluble amine dissolved in an organic solvent, and reacting the resulting oraganic solution with ethylenediamine. The process of the instant invention avoids the use of concentrated nitric acid, as is currently practiced, resulting in a synthesis which is far less hazardous, especially for large quantities of the explosive, and more efficient.

  18. Preparation of ethylenediamine dinitrate

    DOE Patents [OSTI]

    Lee, Kien-yin (Los Alamos, NM)

    1985-01-01

    Method for the preparation of ethylenediamine dinitrate. Ethylenediamine dinitrate, a useful explosive, may readily be prepared by solvent extraction of nitrate ion from an acidic aqueous solution thereof using a high-molecular-weight, water-insoluble amine dissolved in an organic solvent, and reacting the resulting organic solution with ethylenediamine. The process of the instant invention avoids the use of concentrated nitric acid, as is currently practiced, resulting in a synthesis which is far less hazardous especially for large quantities of the explosive, and more efficient.

  19. Preparation of hydrophobic coatings

    DOE Patents [OSTI]

    Branson, Eric D. (Albuquerque, NM); Shah, Pratik B. (Albuquerque, NM); Singh, Seema (Rio Rancho, NM); Brinker, C. Jeffrey (Albuquerque, NM)

    2009-02-03

    A method for preparing a hydrophobic coating by preparing a precursor sol comprising a metal alkoxide, a solvent, a basic catalyst, a fluoroalkyl compound and water, depositing the precursor sol as a film onto a surface, such as a substrate or a pipe, heating, the film and exposing the film to a hydrophobic silane compound to form a hydrophobic coating with a contact angle greater than approximately 150.degree.. The contact angle of the film can be controlled by exposure to ultraviolet radiation to reduce the contact angle and subsequent exposure to a hydrophobic silane compound to increase the contact angle.

  20. ARTICULATION AGREEMENT Teacher Preparation

    E-Print Network [OSTI]

    Hammack, Richard

    ARTICULATION AGREEMENT For Teacher Preparation Between J. Sargeant Reynolds Community College of Interdisciplinary Studies degree in Liberal Studies for Early and Elementary Education (LSEE) and Master of Teaching degree in Elementary Education; · Bachelor of Arts degree in English or History and the Master

  1. Experiments: Preparation and Measurement

    E-Print Network [OSTI]

    Neumaier, Arnold

    the experimental set­up und the results of performing the experiment. Again, this is part of human cultureExperiments: Preparation and Measurement by Arnold Neumaier, Vienna March 1996 Abstract Introduction Experiments, properly arranged, provide information about a physical system by suitable

  2. Preparation of graphitic articles

    DOE Patents [OSTI]

    Phillips, Jonathan; Nemer, Martin; Weigle, John C.

    2010-05-11

    Graphitic structures have been prepared by exposing templates (metal, metal-coated ceramic, graphite, for example) to a gaseous mixture that includes hydrocarbons and oxygen. When the template is metal, subsequent acid treatment removes the metal to yield monoliths, hollow graphitic structures, and other products. The shapes of the coated and hollow graphitic structures mimic the shapes of the templates.

  3. Preparation of vinyl acetate

    DOE Patents [OSTI]

    Tustin, G.C.; Zoeller, J.R.; Depew, L.S.

    1998-03-24

    This invention pertains to the preparation of vinyl acetate by contacting a mixture of hydrogen and ketene with a heterogeneous catalyst containing a transition metal to produce acetaldehyde, which is then reacted with ketene in the presence of an acid catalyst to produce vinyl acetate.

  4. Prepared for Outlook 2020

    E-Print Network [OSTI]

    Northern British Columbia, University of

    Northern British Columbia: A Vision for Prosperity Prepared for Outlook 2020: Shaping BC Trust #12;2 Northern British Columbia's Vision for Prosperity Outlook 2020: Shaping BC's Economic and the emerging bio-energy industry..................................... 15 2.2 Mining, oil and gas

  5. Stakeholder Interview Prepared for

    E-Print Network [OSTI]

    Interviews By GE Global Research For University of Hawaii Hawaii Natural Energy Institute 1680 East-West RoadStakeholder Interview Report Prepared for U.S. Department of Energy Office of Electricity Delivery and Energy Reliability Under Award No. DE-FC-06NT42847 Task 1. Deliverable #1 ­ Results of Stakeholder

  6. An evaluation of a weight-lifting belt and back injury prevention training class for fleet service clerks 

    E-Print Network [OSTI]

    Reddell, Cheryl Renee?

    1991-01-01

    AN EVALUATION OF A WEIGHT-LIFTING BELT AND BACK INJURY PREVENTION TRAINING CLASS FOR FLEET SERVICE CLERKS A Thesis by CHERYL RENEE REDDELL 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 1991 Major Subject: Industrial Engineering AN EVALUATION OF A WEIGHT-LIFTING BELT AND BACK INJURY PREVENTION TRAINING CLASS FOR FLEET SERVICE CLERKS A Thesis by Cheryl Rene' Reddell Approved...

  7. Volterra network modeling of the nonlinear finite-impulse reponse of the radiation belt flux

    SciTech Connect (OSTI)

    Taylor, M.; Daglis, I. A.; Anastasiadis, A. [Institute for Space Applications and Remote Sensing(ISARS), National Observatory of Athens (NOA), Metaxa and Vasillis Pavlou Street, Penteli, Athens 15236 (Greece); Vassiliadis, D. [Department of Physics, Hodges Hall, PO Box 6315, West Virginia University, Morgantown, WV 26506-6315 (United States)

    2011-01-04

    We show how a general class of spatio-temporal nonlinear impulse-response forecast networks (Volterra networks) can be constructed from a taxonomy of nonlinear autoregressive integrated moving average with exogenous inputs (NAR-MAX) input-output equations, and used to model the evolution of energetic particle f uxes in the Van Allen radiation belts. We present initial results for the nonlinear response of the radiation belts to conditions a month earlier. The essential features of spatio-temporal observations are recovered with the model echoing the results of state space models and linear f nite impulse-response models whereby the strongest coupling peak occurs in the preceding 1-2 days. It appears that such networks hold promise for the development of accurate and fully data-driven space weather modelling, monitoring and forecast tools.

  8. THE NUCLEUS OF MAIN-BELT COMET 259P/GARRADD

    SciTech Connect (OSTI)

    MacLennan, Eric M.; Hsieh, Henry H. E-mail: emaclenn@utk.edu

    2012-10-10

    We present observations of the main-belt comet 259P/Garradd, previously known as P/2008 R1 (Garradd), obtained in 2011 and 2012 using the Gemini North Telescope on Mauna Kea in Hawaii and the SOAR telescope at Cerro Pachon in Chile, with the goal of computing the object's phase function and nucleus size. We find an absolute magnitude of H{sub R} = 19.71 {+-} 0.05 mag and slope parameter of G{sub R} = -0.08 {+-} 0.05 for the inactive nucleus, corresponding to an effective nucleus radius of r{sub e} = 0.30 {+-} 0.02 km, assuming an R-band albedo of p{sub R} = 0.05. We also revisit observations reported for 259P while it was active in 2008 to quantify the dust mass loss and compare the object with other known main-belt comets.

  9. THE EXTRAORDINARY MULTI-TAILED MAIN-BELT COMET P/2013 P5

    SciTech Connect (OSTI)

    Jewitt, David [Department of Earth and Space Sciences, University of California at Los Angeles, 595 Charles Young Drive East, Los Angeles, CA 90095-1567 (United States); Agarwal, Jessica [Max Planck Institute for Solar System Research, Max-Planck-Str. 2, D-37191 Katlenburg-Lindau (Germany); Weaver, Harold [The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723 (United States); Mutchler, Max [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Larson, Stephen, E-mail: jewitt@ucla.edu [Lunar and Planetary Laboratory, University of Arizona, 1629 East University Boulevard, Tucson, AZ 85721-0092 (United States)

    2013-11-20

    Hubble Space Telescope observations of main-belt comet P/2013 P5 reveal an extraordinary system of six dust tails that distinguish this object from any other. Observations two weeks apart show dramatic morphological change in the tails while providing no evidence for secular fading of the object as a whole. Each tail is associated with a unique ejection date, revealing continued, episodic mass loss from the 0.24 ± 0.04 km radius nucleus over the last five months. As an inner-belt asteroid and probable Flora family member, the object is likely to be highly metamorphosed and unlikely to contain ice. The protracted period of dust release appears inconsistent with an impact origin, but may be compatible with a body that is losing mass through a rotational instability. We suggest that P/2013 P5 has been accelerated to breakup speed by radiation torques.

  10. The Gould's Belt very large array survey. III. The Orion region

    SciTech Connect (OSTI)

    Kounkel, Marina; Hartmann, Lee [Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109 (United States); Loinard, Laurent; Ortiz-León, Gisela N.; Rodríguez, Luis F.; Pech, Gerardo; Rivera, Juana L. [Centro de Radiostronomía y Astrofísica, Universidad Nacional Autónoma de Mexico, Morelia 58089 (Mexico); Mioduszewski, Amy J. [National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801 (United States); Dzib, Sergio A. [Max Planck Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn (Germany); Torres, Rosa M. [Instituto de Astronomía y Meteorología, Universidad de Guadalajara, Avenida Vallarta No. 2602, Col. Arcos Vallarta, CP 44130, Guadalajara, Jalisco (Mexico); Boden, Andrew F. [Division of Physics, Math and Astronomy, California Institute of Technology, 1200 E California Blvd., Pasadena, CA 91125 (United States); Evans, Neal J. II [Department of Astronomy, The University of Texas at Austin, 1 University Station, C1400, Austin, TX 78712 (United States); Briceño, Cesar [Cerro Tololo Interamerican Observatory, Casilla 603, La Serena (Chile); Tobin, John [National Radio Astronomy Observatory, Charlottesville, VA 22903 (United States)

    2014-07-20

    We present results from a high-sensitivity (60 ?Jy), large-scale (2.26 deg{sup 2}) survey obtained with the Karl G. Jansky Very Large Array as part of the Gould's Belt Survey program. We detected 374 and 354 sources at 4.5 and 7.5 GHz, respectively. Of these, 148 are associated with previously known young stellar objects (YSOs). Another 86 sources previously unclassified at either optical or infrared wavelengths exhibit radio properties that are consistent with those of young stars. The overall properties of our sources at radio wavelengths such as their variability and radio to X-ray luminosity relation are consistent with previous results from the Gould's Belt Survey. Our detections provide target lists for follow-up Very Long Baseline Array radio observations to determine their distances as YSOs are located in regions of high nebulosity and extinction, making it difficult to measure optical parallaxes.

  11. Online monitoring of a belt grinding process by using a light scattering method

    SciTech Connect (OSTI)

    Boehm, Johannes; Vernes, Andras; Vorlaufer, Georg; Vellekoop, Michael

    2010-10-20

    Industrially ground surfaces often have a characteristic surface topography known as chatter marks. The surface finishing is mainly monitored by optical measurement techniques. In this work, the monitoring of an industrial belt grinding process with a light scattering sensor is presented. Although this technique is primarily applied for parametric surface roughness analysis, here it is shown that it enables also the measurement of the surface topography, i.e., the chatter marks occurring during the belt grinding process. In particular, it is proven that the light scattering method is appropriate to measure online the topography of chatter marks. Furthermore, the frequency analysis of the data reveals that the wavelength of chatter marks strongly depends on process parameters, such as the grinding speed.

  12. ANNEALED MYLONITES OF THE SAINT NICHOLAS THRUST (SNT) FROM A NEW EXCAVATION AT THE NEW YORK BOTANICAL GARDENS, THE BRONX, NEW

    E-Print Network [OSTI]

    Merguerian, Charles

    ANNEALED MYLONITES OF THE SAINT NICHOLAS THRUST (SNT) FROM A NEW EXCAVATION AT THE NEW YORK BOTANICAL GARDENS, THE BRONX, NEW YORK Charles Merguerian and John E. Sanders Geology Department, Hofstra Paleozoic rocks of New York City consist of three lithologically distinct amphibolite-grade rock sequences

  13. A SOUTHERN SKY AND GALACTIC PLANE SURVEY FOR BRIGHT KUIPER BELT OBJECTS

    SciTech Connect (OSTI)

    Sheppard, Scott S.; Udalski, Andrzej; Kubiak, Marcin; Pietrzynski, Grzegorz; Poleski, Radoslaw; Soszynski, Igor; Szymanski, Michal K.; Ulaczyk, Krzysztof; Trujillo, Chadwick

    2011-10-15

    About 2500 deg{sup 2} of sky south of declination -25{sup 0} and/or near the Galactic Plane were surveyed for bright outer solar system objects. This survey is one of the first large-scale southern sky and Galactic Plane surveys to detect dwarf planets and other bright Kuiper Belt Objects in the trans-Neptunian region. The survey was able to obtain a limiting R-band magnitude of 21.6. In all, 18 outer solar system objects were detected, including Pluto which was detected near the Galactic center using optimal image subtraction techniques to remove the high stellar density background. Fourteen of the detections were previously unknown trans-Neptunian objects, demonstrating that the southern sky had not been well searched to date for bright outer solar system objects. Assuming moderate albedos, several of the new discoveries from this survey could be in hydrostatic equilibrium and thus could be considered dwarf planets. Combining this survey with previous surveys from the northern hemisphere suggests that the Kuiper Belt is nearly complete to around 21st magnitude in the R band. All the main dynamical classes in the Kuiper Belt are occupied by at least one dwarf-planet-sized object. The 3:2 Neptune resonance, which is the innermost well-populated Neptune resonance, has several large objects while the main outer Neptune resonances such as the 5:3, 7:4, 2:1, and 5:2 do not appear to have any large objects. This indicates that the outer resonances are either significantly depleted in objects relative to the 3:2 resonance or have a significantly different assortment of objects than the 3:2 resonance. For the largest objects (H < 4.5 mag), the scattered disk population appears to have a few times more objects than the main Kuiper Belt (MKB) population, while the Sedna population could be several times more than that of the MKB.

  14. SECULAR RESONANCE SWEEPING OF THE MAIN ASTEROID BELT DURING PLANET MIGRATION

    SciTech Connect (OSTI)

    Minton, David A. [Southwest Research Institute and NASA Lunar Science Institute, 1050 Walnut St., Suite 300, Boulder, CO 80302 (United States); Malhotra, Renu, E-mail: daminton@boulder.swri.edu, E-mail: renu@lpl.arizona.edu [Department of Planetary Sciences, University of Arizona, 1629 East University Boulevard, Tucson, AZ 85721 (United States)

    2011-05-01

    We calculate the eccentricity excitation of asteroids produced by the sweeping {nu}{sub 6} secular resonance during the epoch of planetesimal-driven giant planet migration in the early history of the solar system. We derive analytical expressions for the magnitude of the eccentricity change and its dependence on the sweep rate and on planetary parameters; the {nu}{sub 6} sweeping leads to either an increase or a decrease of eccentricity depending on an asteroid's initial orbit. Based on the slowest rate of {nu}{sub 6} sweeping that allows a remnant asteroid belt to survive, we derive a lower limit on Saturn's migration speed of {approx}0.15 AU Myr{sup -1} during the era that the {nu}{sub 6} resonance swept through the inner asteroid belt (semimajor axis range 2.1-2.8 AU). This rate limit is for Saturn's current eccentricity and scales with the square of its eccentricity; the limit on Saturn's migration rate could be lower if its eccentricity were lower during its migration. Applied to an ensemble of fictitious asteroids, our calculations show that a prior single-peaked distribution of asteroid eccentricities would be transformed into a double-peaked distribution due to the sweeping of the {nu}{sub 6} resonance. Examination of the orbital data of main belt asteroids reveals that the proper eccentricities of the known bright (H {<=} 10.8) asteroids may be consistent with a double-peaked distribution. If so, our theoretical analysis then yields two possible solutions for the migration rate of Saturn and for the dynamical states of the pre-migration asteroid belt: a dynamically cold state (single-peaked eccentricity distribution with mean of {approx}0.05) linked with Saturn's migration speed {approx}4 AU Myr{sup -1} or a dynamically hot state (single-peaked eccentricity distribution with mean of {approx}0.3) linked with Saturn's migration speed {approx}0.8 AU Myr{sup -1}.

  15. A density-temperature description of the outer electron radiation belt during geomagnetic storms

    SciTech Connect (OSTI)

    Borovsky, Joseph E [Los Alamos National Laboratory; Cayton, Thomas E [Los Alamos National Laboratory; Denton, Michael H [LANCASTER UNIV

    2009-01-01

    Electron flux measurements from 7 satellites in geosynchronous orbit from 1990-2007 are fit with relativistic bi-Maxwellians, yielding a number density n and temperature T description of the outer electron radiation belt. For 54.5 spacecraft years of measurements the median value ofn is 3.7x10-4 cm-3 and the median value ofT is 142 keY. General statistical properties of n, T, and the 1.1-1.5 MeV flux J are investigated, including local-time and solar-cycle dependencies. Using superposed-epoch analysis triggered on storm onset, the evolution of the outer electron radiation belt through high-speed-steam-driven storms is investigated. The number density decay during the calm before the storm is seen, relativistic-electron dropouts and recoveries from dropout are investigated, and the heating of the outer electron radiation belt during storms is examined. Using four different triggers (SSCs, southward-IMF CME sheaths, southward-IMF magnetic clouds, and minimum Dst), CME-driven storms are analyzed with superposed-epoch techniques. For CME-driven storms an absence of a density decay prior to storm onset is found, the compression of the outer electron radiation belt at time of SSC is analyzed, the number-density increase and temperature decrease during storm main phase is seen, and the increase in density and temperature during storm recovery phase is observed. Differences are found between the density-temperature and the flux descriptions, with more information for analysis being available in the density-temperature description.

  16. Direct Imaging and Spectroscopy of a Young Extrasolar Kuiper Belt in the Nearest OB Association

    E-Print Network [OSTI]

    Currie, Thayne; Kuchner, Marc J; Madhusudhan, Nikku; Kenyon, Scott J; Thalmann, Christian; Carson, Joseph; Debes, John H

    2015-01-01

    We describe the discovery of a bright, young Kuiper belt-like debris disk around HD 115600, a $\\sim$ 1.4--1.5 M$_\\mathrm{\\odot}$, $\\sim$ 15 Myr old member of the Sco-Cen OB Association. Our H-band coronagraphy/integral field spectroscopy from the \\textit{Gemini Planet Imager} shows the ring has a (luminosity scaled) semi major axis of ($\\sim$ 22 AU) $\\sim$ 48 AU, similar to the current Kuiper belt. The disk appears to have neutral scattering dust, is eccentric (e $\\sim$ 0.1--0.2), and could be sculpted by analogues to the outer solar system planets. Spectroscopy of the disk ansae reveal a slightly blue to gray disk color, consistent with major Kuiper belt chemical constituents, where water-ice is a very plausible dominant constituent. Besides being the first object discovered with the next generation of extreme adaptive optics systems (i.e. SCExAO, GPI, SPHERE), HD 115600's debris ring and planetary system provides a key reference point for the early evolution of the solar system, the structure and compositio...

  17. The Reactivation of Main-Belt Comet 324P/La Sagra (P/2010 R2)

    E-Print Network [OSTI]

    Hsieh, Henry H

    2015-01-01

    We present observations using the Baade Magellan and Canada-France-Hawaii telescopes showing that main-belt comet 324P/La Sagra, formerly known as P/2010 R2, has become active again for the first time since originally observed to be active in 2010-2011. The object appears point-source-like in March and April 2015 as it approached perihelion (true anomaly of ~300 deg), but was ~1 mag brighter than expected if inactive, suggesting the presence of unresolved dust emission. Activity was confirmed by observations of a cometary dust tail in May and June 2015. We find an apparent net dust production rate of belt comet confirmed to be recurrently active, a strong indication that its activity is driven by sublimation. It now has the largest confirmed active range of all likely main-belt comets, and also the most distant confirmed inbound activation point at R~2.8 AU. Further observations during the current active period will allow direct comparisons o...

  18. The New Horizons Pluto Kuiper belt Mission: An Overview with Historical Context

    E-Print Network [OSTI]

    S. Alan Stern

    2007-09-27

    NASA's New Horizons (NH) Pluto-Kuiper belt (PKB) mission was launched on 19 January 2006 on a Jupiter Gravity Assist (JGA) trajectory toward the Pluto system for a 14 July 2015 closest approach; Jupiter closest approach occurred on 28 February 2007. It was competitively selected by NASA for development on 29 November 2001. New Horizons is the first mission to the Pluto system and the Kuiper belt; and will complete the reconnaissance of the classical planets. The ~400 kg spacecraft carries seven scientific instruments, including imagers, spectrometers, radio science, a plasma and particles suite, and a dust counter built by university students. NH will study the Pluto system over a 5-month period beginning in early 2015. Following Pluto, NH will go on to reconnoiter one or two 30-50 kilometer diameter Kuiper belt Objects (KBOs), if NASA approves an extended mission. If successful, NH will represent a watershed development in the scientific exploration of a new class of bodies in the solar system - dwarf planets, of worlds with exotic volatiles on their surfaces, of rapidly (possibly hydrodynamically) escaping atmospheres, and of giant impact derived satellite systems. It will also provide the first dust density measurements beyond 18 AU, cratering records that shed light on both the ancient and present-day KB impactor population down to tens of meters, and a key comparator to the puzzlingly active, former dwarf planet (now satellite of Neptune) called Triton, which is as large as Eris and Pluto.

  19. A POSSIBLE DIVOT IN THE SIZE DISTRIBUTION OF THE KUIPER BELT'S SCATTERING OBJECTS

    SciTech Connect (OSTI)

    Shankman, C.; Gladman, B. J. [Department of Physics and Astronomy, University of British Columbia, 6224 Agriculture Road, Vancouver, BC V6T 1Z1 (Canada); Kaib, N. [Department of Physics and Astronomy, Queens University (Canada); Kavelaars, J. J. [National Research Council of Canada, Victoria, BC V9E 2E7 (Canada); Petit, J. M. [Institut UTINAM, CNRS-Universite de Franche-Comte, Besancon (France)

    2013-02-10

    Via joint analysis of a calibrated telescopic survey, which found scattering Kuiper Belt objects, and models of their expected orbital distribution, we explore the scattering-object (SO) size distribution. Although for D > 100 km the number of objects quickly rise as diameters decrease, we find a relative lack of smaller objects, ruling out a single power law at greater than 99% confidence. After studying traditional ''knees'' in the size distribution, we explore other formulations and find that, surprisingly, our analysis is consistent with a very sudden decrease (a divot) in the number distribution as diameters decrease below 100 km, which then rises again as a power law. Motivated by other dynamically hot populations and the Centaurs, we argue for a divot size distribution where the number of smaller objects rises again as expected via collisional equilibrium. Extrapolation yields enough kilometer-scale SOs to supply the nearby Jupiter-family comets. Our interpretation is that this divot feature is a preserved relic of the size distribution made by planetesimal formation, now ''frozen in'' to portions of the Kuiper Belt sharing a ''hot'' orbital inclination distribution, explaining several puzzles in Kuiper Belt science. Additionally, we show that to match today's SO inclination distribution, the supply source that was scattered outward must have already been vertically heated to the of order 10 Degree-Sign .

  20. PROPERTIES OF THE DISTANT KUIPER BELT: RESULTS FROM THE PALOMAR DISTANT SOLAR SYSTEM SURVEY

    SciTech Connect (OSTI)

    Schwamb, Megan E.; Brown, Michael E. [Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125 (United States); Rabinowitz, David L. [Department of Physics, Yale University, P.O. Box 208121, New Haven, CT 06520 (United States); Ragozzine, Darin, E-mail: mschwamb@gps.caltech.ed [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States)

    2010-09-10

    We present the results of a wide-field survey using the 1.2 m Samuel Oschin Telescope at Palomar Observatory. This survey was designed to find the most distant members of the Kuiper Belt and beyond. We searched {approx}12,000 deg{sup 2} down to a mean limiting magnitude of 21.3 in R. A total number of 52 Kuiper Belt objects and Centaurs have been detected, 25 of which were discovered in this survey. Except for the redetection of Sedna, no additional Sedna-like bodies with perihelia greater than 45 AU were detected despite sensitivity out to distances of 1000 AU. We discuss the implications for a distant Sedna-like population beyond the Kuiper Belt, focusing on the constraints we can place on the embedded stellar cluster environment the early Sun may be have been born in, where the location and distribution of Sedna-like orbits sculpted by multiple stellar encounters is indicative of the birth cluster size. We also report our observed latitude distribution and implications for the size of the plutino population.

  1. RESEARCH ARTICLE 10.1002/2014GC005450

    E-Print Network [OSTI]

    Kaus, Boris

    to folding-dominated fold- and-thrust belt systems, detached over weak basal layers, such as the Zagros

  2. Do variations in Arabian plate lithospheric structure control deformation in the Arabian-Eurasian convergence zone?

    E-Print Network [OSTI]

    Stern, Robert J.

    differently along strike. Subduction north of the Persian Gulf forms the Zagros fold-and-thrust belt

  3. Porous electrode preparation method

    DOE Patents [OSTI]

    Arons, R.M.; Dusek, J.T.

    1983-10-18

    A porous sintered plaque is provided with a bimodal porosity that is especially well suited for use as an electrode within a molten carbonate fuel cell. The coarse porosity is sufficient for admitting gases into contact with the reaction surfaces while the fine porosity is wetted with and retains molten electrolyte on the reaction sites. The electrode structure is prepared by providing a very fine powder of such as nickel oxide and blending the powder with a suitable decomposable binder to form a solid mass. The mass is comminuted into agglomerate size particles substantially larger than the fine oxide particles and formed into a cohesive compact for subsequent sintering. Sintering is carried out at sufficient conditions to bind the agglomerates together into a porous structure having both coarse and fine porosity. Where lithiated nickel oxide cathodes are prepared, the sintering conditions can be moderate enough to retain substantial quantities of lithium within the electrode for adequate conductivity. 2 figs.

  4. Porous electrode preparation method

    DOE Patents [OSTI]

    Arons, Richard M. (Wheaton, IL); Dusek, Joseph T. (Downers Grove, IL)

    1983-01-01

    A porous sintered plaque is provided with a bimodal porosity that is especially well suited for use as an electrode within a molten carbonate fuel cell. The coarse porosity is sufficient for admitting gases into contact with the reaction surfaces while the fine porosity is wetted with and retains molten electrolyte on the reaction sites. The electrode structure is prepared by providing a very fine powder of such as nickel oxide and blending the powder with a suitable decomposable binder to form a solid mass. The mass is comminuted into agglomerate size particles substantially larger than the fine oxide particles and formed into a cohesive compact for subsequent sintering. Sintering is carried out at sufficient conditions to bind the agglomerates together into a porous structure having both coarse and fine porosity. Where lithiated nickel oxide cathodes are prepared, the sintering conditions can be moderate enough to retain substantial quantities of lithium within the electrode for adequate conductivity.

  5. Preparation of fibrous palladium

    SciTech Connect (OSTI)

    Silver, G.L.; Seabaugh, P.W.; Leahy, B.T.; Werkmeister, D.W.; Martin, F.S.; Friedlander, H.N.

    1988-06-15

    Acrylic fibers (pan fibers) absorb palladium from a hot solution of palladium nitrate in nitric acid. When palladium-loaded acrylic fibers are burned, fibers consisting of palladium and palladium oxide are formed. Reduction of this mixture with hydrogen produces fibers of palladium metal. The fibers may be compressed into pellets which offer less resistance to flowing hydrogen than similar pellets prepared by compressing commercial palladium powder. 9 refs., 12 figs., 5 tabs.

  6. TORIS Data Preparation Guidelines

    SciTech Connect (OSTI)

    Guinn, H.; Remson, D.

    1999-03-11

    The objective of this manual is to present guidelines and procedures for the preparation of new data for the Tertiary Oil Recovery Information System (TORIS) data base. TORIS is an analytical system currently maintained by the Department of Energy's (DOE) Bartlesville Project Office. It uses an extensive field- and reservoir-level data base to evaluate the technical and economic recovery potential of specific crude oil reservoirs.

  7. 2007 TY430: A COLD CLASSICAL KUIPER BELT TYPE BINARY IN THE PLUTINO POPULATION

    SciTech Connect (OSTI)

    Sheppard, Scott S.; Ragozzine, Darin; Trujillo, Chadwick

    2012-03-15

    Kuiper Belt object 2007 TY430 is the first wide, equal-sized, binary known in the 3:2 mean motion resonance with Neptune. The two components have a maximum separation of about 1 arcsec and are on average less than 0.1 mag different in apparent magnitude with identical ultra-red colors (g - i = 1.49 {+-} 0.01 mag). Using nearly monthly observations of 2007 TY430 from 2007 to 2011, the orbit of the mutual components was found to have a period of 961.2 {+-} 4.6 days with a semi-major axis of 21000 {+-} 160 km and eccentricity of 0.1529 {+-} 0.0028. The inclination with respect to the ecliptic is 15.68 {+-} 0.22 deg and extensive observations have allowed the mirror orbit to be eliminated as a possibility. The total mass for the binary system was found to be 7.90 {+-} 0.21 Multiplication-Sign 10{sup 17} kg. Equal-sized, wide binaries and ultra-red colors are common in the low-inclination 'cold' classical part of the Kuiper Belt and likely formed through some sort of three-body interactions within a much denser Kuiper Belt. To date 2007 TY430 is the only ultra-red, equal-sized binary known outside of the classical Kuiper Belt population. Numerical simulations suggest 2007 TY430 is moderately unstable in the outer part of the 3:2 resonance and thus 2007 TY430 is likely an escaped 'cold' classical object that later got trapped in the 3:2 resonance. Similar to the known equal-sized, wide binaries in the cold classical population, the binary 2007 TY430 requires a high albedo and very low density structure to obtain the total mass found for the pair. For a realistic minimum density of 0.5 g cm{sup -3} the albedo of 2007 TY430 would be greater than 0.17. For reasonable densities, the radii of either component should be less than 60 km, and thus the relatively low eccentricity of the binary is interesting since no tides should be operating on the bodies at their large distances from each other. The low prograde inclination of the binary also makes it unlikely that the Kozai mechanism could have altered the orbit, making the 2007 TY430 binary orbit likely one of the few relatively unaltered primordial binary orbits known. Under some binary formation models, the low-inclination prograde orbit of the 2007 TY430 binary indicates formation within a relatively high velocity regime in the Kuiper Belt.

  8. THE COLOR DIFFERENCES OF KUIPER BELT OBJECTS IN RESONANCE WITH NEPTUNE

    SciTech Connect (OSTI)

    Sheppard, Scott S.

    2012-12-01

    The optical colors of 58 objects in mean motion resonance with Neptune were obtained. The various Neptune resonant populations were found to have significantly different surface color distributions. The 5:3 and 7:4 resonances have semimajor axes near the middle of the main Kuiper Belt and both are dominated by ultra-red material (spectral gradient: S {approx}> 25). The 5:3 and 7:4 resonances have statistically the same color distribution as the low-inclination 'cold' classical belt. The inner 4:3 and distant 5:2 resonances have objects with mostly moderately red colors (S {approx} 15), similar to the scattered and detached disk populations. The 2:1 resonance, which is near the outer edge of the main Kuiper Belt, has a large range of colors with similar numbers of moderately red and ultra-red objects at all inclinations. The 2:1 resonance was also found to have a very rare neutral colored object showing that the 2:1 resonance is really a mix of all object types. The inner 3:2 resonance, like the outer 2:1, has a large range of objects from neutral to ultra-red. The Neptune Trojans (1:1 resonance) are only slightly red (S {approx} 9), similar to the Jupiter Trojans. The inner 5:4 resonance only has four objects with measured colors but shows equal numbers of ultra-red and moderately red objects. The 9:5, 12:5, 7:3, 3:1, and 11:3 resonances do not have reliable color distribution statistics since few objects have been observed in these resonances, though it appears noteworthy that all three of the measured 3:1 objects have only moderately red colors, similar to the 4:3 and 5:2 resonances. The different color distributions of objects in mean motion resonance with Neptune are likely a result from the disruption of the primordial Kuiper Belt from the scattering and migration of the giant planets. The few low-inclination objects known in the outer 2:1 and 5:2 resonances are mostly only moderately red. This suggests if the 2:1 and 5:2 have a cold low-inclination component, the objects likely had a significantly different origin than the ultra-red-dominated cold components of the cold classical belt and 5:3 and 7:4 resonances.

  9. THE CANADA-FRANCE ECLIPTIC PLANE SURVEY-L3 DATA RELEASE: THE ORBITAL STRUCTURE OF THE KUIPER BELT

    SciTech Connect (OSTI)

    Kavelaars, J. J.; Jones, R. L.; Murray, I. [Herzberg Institute of Astrophysics, National Research Council of Canada, Victoria, BC V9E 2E7 (Canada); Gladman, B. J.; Petit, J.-M.; Van Laerhoven, C. [Department of Physics and Astronomy, 6224 Agricultural Road, University of British Columbia, Vancouver, BC (Canada); Parker, Joel Wm.; Bieryla, A. [Space Science and Engineering Division, Southwest Research Institute, 1050 Walnut Street, Suite 400, Boulder, CO 80302 (United States); Nicholson, P.; Margot, J. L. [Cornell University, Space Sciences Building, Ithaca, NY 14853 (United States); Rousselot, P.; Mousis, O. [Institut UTINAM, CNRS-UMR 6213, Observatoire de Besancon, BP 1615, 25010 Besancon Cedex (France); Scholl, H. [Observatoire de la Cote d'Azur, BP 4229, Boulevard de l'Observatoire, F-06304 Nice Cedex 4 (France); Marsden, B. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Benavidez, P.; Campo Bagatin, A. [Departamento de Fisica, Ingenieria de Sistemas y Teoria de la Senal, E.P.S.A., Universidad de Alicante, Apartado de Correos 99, Alicante 03080 (Spain); Doressoundiram, A. [LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex (France); Veillet, C. [Canada-France-Hawaii Telescope Corporation, P.O. Box 1597, Kamuela, HI 96743 (United States)

    2009-06-15

    We report the orbital distribution of the trans-Neptunian comets discovered during the first discovery year of the Canada-France Ecliptic Plane Survey (CFEPS). CFEPS is a Kuiper Belt object survey based on observations acquired by the Very Wide component of the Canada-France-Hawaii Telescope Legacy Survey (LS-VW). The first year's detections consist of 73 Kuiper Belt objects, 55 of which have now been tracked for three years or more, providing precise orbits. Although this sample size is small compared to the world-wide inventory, because we have an absolutely calibrated and extremely well-characterized survey (with known pointing history) we are able to de-bias our observed population and make unbiased statements about the intrinsic orbital distribution of the Kuiper Belt. By applying the (publically available) CFEPS Survey Simulator to models of the true orbital distribution and comparing the resulting simulated detections to the actual detections made by the survey, we are able to rule out several hypothesized Kuiper Belt object orbit distributions. We find that the main classical belt's so-called 'cold' component is confined in semimajor axis (a) and eccentricity (e) compared to the more extended 'hot' component; the cold component is confined to lower e and does not stretch all the way out to the 2:1 resonance but rather depletes quickly beyond a = 45 AU. For the cold main classical belt population we find a robust population estimate of N(H{sub g} < 10) = 50 {+-} 5 x 10{sup 3} and find that the hot component of the main classical belt represents {approx}60% of the total population. The inner classical belt (sunward of the 3:2 mean-motion resonance) has a population of roughly 2000 trans-Neptunian objects with absolute magnitudes H{sub g} < 10, and may not share the inclination distribution of the main classical belt. We also find that the plutino population lacks a cold low-inclination component, and so, the population is somewhat larger than recent estimates; our analysis shows a plutino population of N(H{sub g} < 10){approx} 25{sup +25} {sub -12} x 10{sup 3}compared to our estimate of the size of main classical Kuiper Belt population of N(H{sub g} < 10) {approx} (126{sup +50} {sub -46}) x 10{sup 3}.

  10. Brown, E.H., Housen, B.A., and Schermer, E.R., 2007, Tectonic evolution of the San Juan Islands thrust system, Washington, in Stelling, P., and Tucker, D.S., eds., Floods, Faults, and Fire: Geological Field Trips in Washington State and Southwest British

    E-Print Network [OSTI]

    Housen, Bernie

    convergent margin tectonism. The area is underlain by the San Juan Islands­northwest Cascades thrust system, dispersal and final emplacement of terranes of the San Juan Islands­northwest Cascades thrust system evolution of the San Juan Islands thrust system, Washington E.H. Brown B.A. Housen E.R. Schermer Department

  11. Preparation of tungsten oxide

    DOE Patents [OSTI]

    Bulian, Christopher J. (Yankton, SD); Dye, Robert C. (Los Alamos, NM); Son, Steven F. (Los Alamos, NM); Jorgensen, Betty S. (Jemez Springs, NM); Perry, W. Lee (Jemez Springs, NM)

    2009-09-22

    Tungsten trioxide hydrate (WO.sub.3.H.sub.2O) was prepared from a precursor solution of ammonium paratungstate in concentrated aqueous hydrochloric acid. The precursor solution was rapidly added to water, resulting in the crash precipitation of a yellow white powder identified as WO.sub.3.H.sub.2O nanosized platelets by x-ray diffraction and scanning electron microscopy. Annealing of the powder at 200.degree. C. provided cubic phase WO.sub.3 nanopowder, and at 400.degree. C. provided WO.sub.3 nanopowder as a mixture of monoclinic and orthorhombic phases.

  12. THE CANADA-FRANCE ECLIPTIC PLANE SURVEY-FULL DATA RELEASE: THE ORBITAL STRUCTURE OF THE KUIPER BELT

    SciTech Connect (OSTI)

    Petit, J.-M.; Rousselot, P.; Mousis, O. [Institut UTINAM, CNRS-UMR 6213, Observatoire de Besancon, BP 1615, 25010 Besancon Cedex (France); Kavelaars, J. J. [Herzberg Institute of Astrophysics, National Research Council of Canada, Victoria, BC V9E 2E7 (Canada); Gladman, B. J.; Jones, R. L.; Van Laerhoven, C. [Department of Physics and Astronomy, University of British Columbia, Vancouver, BC (Canada); Parker, J. Wm.; Bieryla, A. [Planetary Science Directorate, Southwest Research Institute, Boulder, CO 80302 (United States); Nicholson, P. [Department of Astronomy, Cornell University, Space Sciences Building, Ithaca, NY 14853 (United States); Mars, G. [Observatoire de la Cote d'Azur, BP 4229, F-06304 Nice Cedex 4 (France); Marsden, B.; Ashby, M. L. N. [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States); Taylor, M.; Bernabeu, G. [Department of Physics and Astronomy, University of Victoria, Victoria, BC V8W 2Y2 (Canada); Benavidez, P.; Campo Bagatin, A. [Departamento de Fisica, Ingenieria de Sistemas y Teoria de la Senal, E.P.S.A., Universidad de Alicante, Apartado de Correos 99, Alicante 03080 (Spain)

    2011-10-15

    We report the orbital distribution of the trans-Neptunian objects (TNOs) discovered during the Canada-France Ecliptic Plane Survey (CFEPS), whose discovery phase ran from early 2003 until early 2007. The follow-up observations started just after the first discoveries and extended until late 2009. We obtained characterized observations of 321 deg{sup 2} of sky to depths in the range g {approx} 23.5-24.4 AB mag. We provide a database of 169 TNOs with high-precision dynamical classification and known discovery efficiency. Using this database, we find that the classical belt is a complex region with sub-structures that go beyond the usual splitting of inner (interior to 3:2 mean-motion resonance [MMR]), main (between 3:2 and 2:1 MMR), and outer (exterior to 2:1 MMR). The main classical belt (a = 40-47 AU) needs to be modeled with at least three components: the 'hot' component with a wide inclination distribution and two 'cold' components (stirred and kernel) with much narrower inclination distributions. The hot component must have a significantly shallower absolute magnitude (H{sub g} ) distribution than the other two components. With 95% confidence, there are 8000{sup +1800}{sub -1600} objects in the main belt with H{sub g} {<=} 8.0, of which 50% are from the hot component, 40% from the stirred component, and 10% from the kernel; the hot component's fraction drops rapidly with increasing H{sub g} . Because of this, the apparent population fractions depend on the depth and ecliptic latitude of a trans-Neptunian survey. The stirred and kernel components are limited to only a portion of the main belt, while we find that the hot component is consistent with a smooth extension throughout the inner, main, and outer regions of the classical belt; in fact, the inner and outer belts are consistent with containing only hot-component objects. The H{sub g} {<=} 8.0 TNO population estimates are 400 for the inner belt and 10,000 for the outer belt to within a factor of two (95% confidence). We show how the CFEPS Survey Simulator can be used to compare a cosmogonic model for the orbital element distribution to the real Kuiper Belt.

  13. Towards a dynamics-based estimate of the extent of HR 8799's unresolved warm debris belt

    E-Print Network [OSTI]

    Contro, B; Horner, J; Marshall, J P

    2015-01-01

    In many ways, the HR8799 system resembles our Solar system more closely than any other discovered to date - albeit on a larger, younger, and more dramatic scale - featuring four giant planets and two debris belts. The first belt lies beyond the orbit of the outer planet, and mirrors our Solar system's Edgeworth-Kuiper belt. The second belt lies interior to the orbit of the inner planet, HR8799e, and is analogous to our Asteroid Belt. With such a similar architecture, the system is a valuable laboratory for examining exoplanet dynamics, and the interaction between debris disks and planets. In recent years, HR8799's outer disk has been relatively well characterised, primarily using the Herschel Space Observatory. In contrast, the inner disk, too close to HR8799 to be spatially resolved by Herschel, remains poorly understood. This leaves significant questions over both the location of the planetesimals responsible for producing the observed dust, and the physical properties of those grains. We have performed ext...

  14. The impact of main belt asteroids on infrared--submillimetre photometry and source counts

    E-Print Network [OSTI]

    Cs. Kiss; A. Pal; Th. G. Mueller; P. Abraham

    2007-11-28

    > Among the components of the infrared and submillimetre sky background, the closest layer is the thermal emission of dust particles and minor bodies in the Solar System. This contribution is especially important for current and future infrared and submillimetre space instruments --like those of Spitzer, Akari and Herschel -- and must be characterised by a reliable statistical model. > We describe the impact of the thermal emission of main belt asteroids on the 5...1000um photometry and source counts, for the current and future spaceborne and ground-based instruments, in general, as well as for specific dates and sky positions. > We used the statistical asteroid model (SAM) to calculate the positions of main belt asteroids down to a size of 1km, and calculated their infrared and submillimetre brightness using the standard thermal model. Fluctuation powers, confusion noise values and number counts were derived from the fluxes of individual asteroids. > We have constructed a large database of infrared and submillimetre fluxes for SAM asteroids with a temporal resolution of 5 days, covering the time span January 1, 2000 -- December 31, 2012. Asteroid fluctuation powers and number counts derived from this database can be obtained for a specific observation setup via our public web-interface. > Current space instruments working in the mid-infrared regime (Akari and Spitzer Space Telescopes) are affected by asteroid confusion noise in some specific areas of the sky, while the photometry of space infrared and submillimetre instruments in the near future (e.g. Herschel and Planck Space Observatories) will not be affected by asteroids. Faint main belt asteroids might also be responsible for most of the zodiacal emission fluctuations near the ecliptic.

  15. CHARACTERIZATION OF ACTIVE MAIN BELT OBJECT P/2012 F5 (GIBBS): A POSSIBLE IMPACTED ASTEROID

    SciTech Connect (OSTI)

    Stevenson, R.; Kramer, E. A.; Bauer, J. M.; Masiero, J. R.; Mainzer, A. K., E-mail: Rachel.A.Stevenson@jpl.nasa.gov [Jet Propulsion Laboratory, Caltech, 4800 Oak Grove Drive, Pasadena, CA 91109 (United States)

    2012-11-10

    In this work, we characterize the recently discovered active main belt object P/2012 F5 (Gibbs), which was discovered with a dust trail >7' in length in the outer main belt, 7 months prior to aphelion. We use optical imaging obtained on UT 2012 March 27 to analyze the central condensation and the long trail. We find B-band and R-band apparent magnitudes of 20.96 {+-} 0.04 mag and 19.93 {+-} 0.02 mag, respectively, which give an upper limit on the radius of the nucleus of 2.1 km. The geometric scattering cross-section of material in the trail was {approx}4 Multiplication-Sign 10{sup 8} m{sup 2}, corresponding to a mass of {approx}5 Multiplication-Sign 10{sup 7} kg. Analysis of infrared images taken by the Wide-field Infrared Survey Explorer in 2010 September reveals that the object was below the detection limit, suggesting that it was less active than it was during 2012, or possibly inactive, just six months after it passed through perihelion. We set a 1{sigma} upper limit on its radius during this time of 2.9 km. P/2012 F5 (Gibbs) is dynamically stable in the outer main belt on timescales of {approx}1 Gyr, pointing toward an asteroidal origin. We find that the morphology of the ejected dust is consistent with it being produced by a single event that occurred on UT 2011 July 7 {+-} 20 days, possibly as the result of a collision with a small impactor.

  16. New Horizons Science Photos from NASA's Pluto-Kuiper Belt Mission

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

    DOE provided the power supply for NASA's New Horizons Mission, a mission to the Pluto and Charon, a double-planet system, and the Kuiper Belt. There are 61 science photos posted on the New Horizons website, along with mission photos, spacecraft images, launch photos, posters and renderings that are both scientific and artistic. Dates range from June of 2006 to February of 2008. The images can be searched by keywords, by date, or by subject topic. They can also be browsed as an entire list. Each image has a detailed description.

  17. Method to prepare Semtex

    SciTech Connect (OSTI)

    Alcaraz, A; Dougan, A

    2006-11-26

    This procedure requires the binder and uncoated RDX be prepared in separate steps, see Figure 1: (1) The binder and dye are mixed by agitation with a water-insoluble organic solvent (e.g., toluene), I; (2) The RDX/PETN is agitated thoroughly with water, II; (3) The binder solution I is added to the RDX/water mixture at II with thorough mixing to form a slurry III; (4) In the next step the solvent is distilled off at IV leaving resulting granules; (5) The next step is followed by filtration at V, which may be done by vacuum; (6) The composition is then dried at VI to a dough-like consistency.

  18. Extensional collapse of the northern Taiwan mountain belt Louis S. Teng Department of Geology, National Taiwan University, 245 Choushan Road, Taipei, Taiwan, Republic of China

    E-Print Network [OSTI]

    Lin, Andrew Tien-Shun

    Extensional collapse of the northern Taiwan mountain belt Louis S. Teng Department of Geology, National Taiwan University, 245 Choushan Road, Taipei, Taiwan, Republic of China ABSTRACT As an active collision zone between the Luzon arc and the China continental margin, the Taiwan mountain belt

  19. Environmental Programs Procedure Preparation, Revision, Review...

    Energy Savers [EERE]

    Environmental Programs Procedure Preparation, Revision, Review, Approval, and Use Environmental Programs Procedure Preparation, Revision, Review, Approval, and Use The documents...

  20. On the generation of large amplitude spiky solitons by ultralow frequency earthquake emission in the Van Allen radiation belt

    SciTech Connect (OSTI)

    Mofiz, U. A. [School of Science and Technology, Bangladesh Open University, Gazipur-1705 (Bangladesh)

    2006-08-15

    The parametric coupling between earthquake emitted circularly polarized electromagnetic radiation and ponderomotively driven ion-acoustic perturbations in the Van Allen radiation belt is considered. A cubic nonlinear Schroedinger equation for the modulated radiation envelope is derived, and then solved analytically. For ultralow frequency earthquake emissions large amplitude spiky supersonic bright solitons or subsonic dark solitons are found to be generated in the Van Allen radiation belt, detection of which can be a tool for the prediction of a massive earthquake may be followed later.

  1. Outer irregular satellites of the planets and their relationship with asteroids, comets and Kuiper Belt objects

    E-Print Network [OSTI]

    Scott S. Sheppard

    2006-05-01

    Outer satellites of the planets have distant, eccentric orbits that can be highly inclined or even retrograde relative to the equatorial planes of their planets. These irregular orbits cannot have formed by circumplanetary accretion and are likely products of early capture from heliocentric orbit. The irregular satellites may be the only small bodies remaining which are still relatively near their formation locations within the giant planet region. The study of the irregular satellites provides a unique window on processes operating in the young solar system and allows us to probe possible planet formation mechanisms and the composition of the solar nebula between the rocky objects in the main asteroid belt and the very volatile rich objects in the Kuiper Belt. The gas and ice giant planets all appear to have very similar irregular satellite systems irrespective of their mass or formation timescales and mechanisms. Water ice has been detected on some of the outer satellites of Saturn and Neptune whereas none has been observed on Jupiter's outer satellites.

  2. 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

    2008-07-03

    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.

  3. Dynamical Heating Induced by Dwarf Planets on Cold Kuiper Belt-like Debris Disks

    E-Print Network [OSTI]

    Muñoz-Gutiérrez, Marco A; Reyes-Ruiz, Mauricio; Peimbert, Antonio

    2015-01-01

    With the use of long-term numerical simulations, we study the evolution and orbital behavior of cometary nuclei in cold Kuiper belt-like debris disks under the gravitational influence of dwarf planets (DPs); we carry out these simulations with and without the presence of a Neptune-like giant planet. This exploratory study shows that in the absence of a giant planet, 10 DPs are enough to induce strong radial and vertical heating on the orbits of belt particles. On the other hand, the presence of a giant planet close to the debris disk, acts as a stability agent reducing the radial and vertical heating. With enough DPs, even in the presence of a Neptune-like giant planet some radial heating remains; this heating grows steadily, re-filling resonances otherwise empty of cometary nuclei. Specifically for the solar system, this secular process seems to be able to provide material that, through resonant chaotic diffusion, increase the rate of new comets spiraling into the inner planetary system, but only if more tha...

  4. Models of the Collisional Damping Scenario for Ice Giant Planets and Kuiper Belt Formatio

    E-Print Network [OSTI]

    Harold F. Levison; Alessandro Morbidelli

    2007-01-18

    Chiang et al. 2006, hereafter C06 have recently proposed that the observed structure of the Kuiper belt could be the result of a dynamical instability of a system of ~5 primordial ice giant planets in the outer Solar System. According to this scenario, before the instability occurred, these giants were growing in a highly collisionally damped environment according to the arguments in Goldreich et al. (2004a,b, hereafter G04). Here we test this hypothesis with a series of numerical simulations using a new code designed to incorporate the dynamical effects of collisions. We find that we cannot reproduce the observed Solar System. In particular, G04 and C06 argue that during the instability, all but two of the ice giants would be ejected from the Solar System by Jupiter and Saturn, leaving Uranus and Neptune behind. We find that ejections are actually rare and that instead the systems spread outward. This always leads to a configuration with too many planets that are too far from the Sun. Thus, we conclude that both G04's scheme for the formation of Uranus and Neptune and C06's Kuiper belt formation scenario are not viable in their current forms.

  5. Main-Belt Asteroids in the K2 Engineering Field of View

    E-Print Network [OSTI]

    Szabó, R; Szabó, Gy M; Pál, A; Kiss, Cs P; Csák, B; Illés, L; Rácz, G; Kiss, L L

    2015-01-01

    Unlike NASA's original Kepler Discovery Mission, the renewed K2 Mission will stare at the plane of the Ecliptic, observing each field for approximately 75 days. This will bring new opportunities and challenges, in particular the presence of a large number of main-belt asteroids that will contaminate the photometry. The large pixel size makes K2 data susceptible to the effect of apparent minor planet encounters. Here we investigate the effects of asteroid encounters on photometric precision using a sub-sample of the K2 Engineering data taken in February, 2014. We show examples of asteroid contamination to facilitate their recognition and distinguish these events from other error sources. We conclude that main-belt asteroids will have considerable effects on K2 photometry of a large number of photometric targets during the Mission, that will have to be taken into account. These results will be readily applicable for future space photometric missions applying large-format CCDs, such as TESS and PLATO.

  6. Discovery of a planetary-sized object in the scattered Kuiper belt

    E-Print Network [OSTI]

    M. E. Brown; C. A. Trujillo; D. L. Rabinowitz

    2005-08-30

    We present the discovery and initial physical and dynamical characterization of the object 2003 UB313. The object is sufficiently bright that for all reasonable values of the albedo it is certain to be larger than Pluto. Pre-discovery observations back to 1989 are used to obtain an orbit with extremely small errors. The object is currently at aphelion in what appears to be a typical orbit for a scattered Kuiper belt object except that it is inclined by about 44 degrees from the ecliptic. The presence of such a large object at this extreme inclination suggests that high inclination Kuiper belt objects formed preferentially closer to the sun. Observations from Gemini Observatory show that the infrared spectrum is, like that of Pluto, dominated by the presence of frozen methane, though visible photometry shows that the object is almost neutral in color compared to Pluto's extremely red color. 2003 UB313 is likely to undergo substantial seasonal change over the large range of heliocentric distances that it travels; Pluto at its current distance is likely to prove a useful analog for better understanding the range of seasonal changes on this body.

  7. Main-belt asteroids with WISE/NEOWISE: Near-infrared albedos

    SciTech Connect (OSTI)

    Masiero, Joseph R.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; Sonnett, S. [Jet Propulsion Laboratory/Caltech, 4800 Oak Grove Drive, MS 183-601, Pasadena, CA 91109 (United States); Grav, T., E-mail: Joseph.Masiero@jpl.nasa.gov, E-mail: amainzer@jpl.nasa.gov, E-mail: cnugent@jpl.nasa.gov, E-mail: James.Bauer@jpl.nasa.gov, E-mail: Rachel.A.Stevenson@jpl.nasa.gov, E-mail: sarah.sonnett@jpl.nasa.gov, E-mail: tgrav@psi.edu [Planetary Science Institute, Tucson, AZ (United States)

    2014-08-20

    We present revised near-infrared albedo fits of 2835 main-belt asteroids observed by WISE/NEOWISE over the course of its fully cryogenic survey in 2010. These fits are derived from reflected-light near-infrared images taken simultaneously with thermal emission measurements, allowing for more accurate measurements of the near-infrared albedos than is possible for visible albedo measurements. Because our sample requires reflected light measurements, it undersamples small, low-albedo asteroids, as well as those with blue spectral slopes across the wavelengths investigated. We find that the main belt separates into three distinct groups of 6%, 16%, and 40% reflectance at 3.4 ?m. Conversely, the 4.6 ?m albedo distribution spans the full range of possible values with no clear grouping. Asteroid families show a narrow distribution of 3.4 ?m albedos within each family that map to one of the three observed groupings, with the (221) Eos family being the sole family associated with the 16% reflectance 3.4 ?m albedo group. We show that near-infrared albedos derived from simultaneous thermal emission and reflected light measurements are important indicators of asteroid taxonomy and can identify interesting targets for spectroscopic follow-up.

  8. Process for preparing liquid wastes

    DOE Patents [OSTI]

    Oden, Laurance L. (Albany, OR); Turner, Paul C. (Albany, OR); O'Connor, William K. (Lebanon, OR); Hansen, Jeffrey S. (Corvallis, OR)

    1997-01-01

    A process for preparing radioactive and other hazardous liquid wastes for treatment by the method of vitrification or melting is provided for.

  9. OBSERVATIONAL AND DYNAMICAL CHARACTERIZATION OF MAIN-BELT COMET P/2010 R2 (La Sagra)

    SciTech Connect (OSTI)

    Hsieh, Henry H.; Yang Bin; Haghighipour, Nader; Jedicke, Robert; Wainscoat, Richard J.; Denneau, Larry; Kaluna, Heather M.; Kleyna, Jan [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu HI 96822 (United States); Novakovic, Bojan [Department of Astronomy, Faculty of Mathematics, University of Belgrade, Studentski trg 16, 11000 Belgrade (Serbia); Abe, Shinsuke; Chen Wenping; Ip, Wing; Kinoshita, Daisuke [Institute of Astronomy, National Central University, 300 Jhongda Rd, Jhongli 32001, Taiwan (China); Fitzsimmons, Alan; Lacerda, Pedro [Astronomy Research Centre, Queens University Belfast, Belfast BT7 1NN (United Kingdom); Granvik, Mikael [Department of Physics, P.O. Box 64, 00014 University of Helsinki (Finland); Grav, Tommy [Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218 (United States); Knight, Matthew M. [Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001 (United States); Lisse, Carey M. [Planetary Exploration Group, Space Department, Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723 (United States); Maclennan, Eric, E-mail: hsieh@ifa.hawaii.edu [Department of Physics and Astronomy, Northern Arizona University, 602 South Humphreys Street, Flagstaff, AZ 86011 (United States); and others

    2012-05-15

    We present observations of the recently discovered comet-like main-belt object P/2010 R2 (La Sagra) obtained by Pan-STARRS1 and the Faulkes Telescope-North on Haleakala in Hawaii, the University of Hawaii 2.2 m, Gemini-North, and Keck I telescopes on Mauna Kea, the Danish 1.54 m telescope (operated by the MiNDSTEp consortium) at La Silla, and the Isaac Newton Telescope on La Palma. An antisolar dust tail is observed to be present from 2010 August through 2011 February, while a dust trail aligned with the object's orbit plane is also observed from 2010 December through 2011 August. Assuming typical phase darkening behavior, P/La Sagra is seen to increase in brightness by >1 mag between 2010 August and December, suggesting that dust production is ongoing over this period. These results strongly suggest that the observed activity is cometary in nature (i.e., driven by the sublimation of volatile material), and that P/La Sagra is therefore the most recent main-belt comet to be discovered. We find an approximate absolute magnitude for the nucleus of H{sub R} = 17.9 {+-} 0.2 mag, corresponding to a nucleus radius of {approx}0.7 km, assuming an albedo of p = 0.05. Comparing the observed scattering surface areas of the dust coma to that of the nucleus when P/La Sagra was active, we find dust-to-nucleus area ratios of A{sub d} /A{sub N} = 30-60, comparable to those computed for fellow main-belt comets 238P/Read and P/2008 R1 (Garradd), and one to two orders of magnitude larger than for two other main-belt comets (133P/Elst-Pizarro and 176P/LINEAR). Using optical spectroscopy to search for CN emission, we do not detect any conclusive evidence of sublimation products (i.e., gas emission), finding an upper limit CN production rate of Q{sub CN} < 6 Multiplication-Sign 10{sup 23} mol s{sup -1}, from which we infer an H{sub 2}O production rate of Q{sub H{sub 2O}} < 10{sup 26} mol s{sup -1}. Numerical simulations indicate that P/La Sagra is dynamically stable for >100 Myr, suggesting that it is likely native to its current location and that its composition is likely representative of other objects in the same region of the main belt, though the relatively close proximity of the 13:6 mean-motion resonance with Jupiter and the (3,-2,-1) three-body mean-motion resonance with Jupiter and Saturn mean that dynamical instability on larger timescales cannot be ruled out.

  10. [The Journal of Geology, 2007, volume 115, p. 315334] 2007 by The University of Chicago. All rights reserved. 0022-1376/2007/11503-0004$15.00 Orogenic Belts and Orogenic Sediment Provenance

    E-Print Network [OSTI]

    rights reserved. 0022-1376/2007/11503-0004$15.00 315 Orogenic Belts and Orogenic Sediment Provenance ophiolites, neometamorphic axial belts, accreted paleomargin remnants, and accreted orogenic clastic wedges of sediment provenances (magmatic arc, ophiolite, axial belt, continental block, and clastic wedge provenances

  11. CITIZENSHIP NOW! EXAM PREPARATION HANDBOOK

    E-Print Network [OSTI]

    Qiu, Weigang

    CITIZENSHIP NOW! EXAM PREPARATION HANDBOOK #12;washington oregon nevada idaho montananorthdakota to offer targeted programs--Si Se Puede!, a joint education initiative between CUNY and the Consulate NOW! EXAM PREPARATION HANDBOOK #12;T he City University of New York is the nation's largest urban

  12. Scissor thrust valve actuator

    DOE Patents [OSTI]

    DeWall, Kevin G.; Watkins, John C; Nitzel, Michael E.

    2006-08-29

    Apparatus for actuating a valve includes a support frame and at least one valve driving linkage arm, one end of which is rotatably connected to a valve stem of the valve and the other end of which is rotatably connected to a screw block. A motor connected to the frame is operatively connected to a motor driven shaft which is in threaded screw driving relationship with the screw block. The motor rotates the motor driven shaft which drives translational movement of the screw block which drives rotatable movement of the valve driving linkage arm which drives translational movement of the valve stem. The valve actuator may further include a sensory control element disposed in operative relationship with the valve stem, the sensory control element being adapted to provide control over the position of the valve stem by at least sensing the travel and/or position of the valve stem.

  13. Physics Thrust Areas

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

    Laboratory Directed Research and Development Materials in Extremes Muon Tomography Neuro and Cognitive Sciences Nuclear Physics Nuclear Weapons and Global Security Data...

  14. Physics Thrust Areas

    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: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass mapSpeeding access| DepartmentPeerFederal FleetUp inrd IEEE(Journal Article) |

  15. Wednesday, 06 October, 2010 Contrasting the efficiency of radiation belt losses caused by ducted and non-1

    E-Print Network [OSTI]

    Otago, University of

    Wednesday, 06 October, 2010 1 Contrasting the efficiency of radiation belt losses caused by ducted and non-1 ducted whistler mode waves from ground-based transmitters2 Craig J. Rodger and Bonar R. Carson3 plasmaspheric whistler ducts which guide the waves. For non-guided cases these waves are21 said to be "nonducted

  16. Radial gradients of phase space density of the outer radiation belt electrons prior to sudden solar wind pressure enhancements

    E-Print Network [OSTI]

    Li, Xinlin

    PSD radial gradient at and beyond GEO prior to a sudden solar wind pressure impact based on the fact by a sudden solar wind pressure enhancement, dayside trapped electrons are transported radially inwards), Radial gradients of phase space density of the outer radiation belt electrons prior to sudden solar wind

  17. 1132 OPTICS LETTERS / Vol. 21, No. 15 / August 1, 1996 Optical conveyor belts: a new scheme for

    E-Print Network [OSTI]

    Miller, Peter D.

    1132 OPTICS LETTERS / Vol. 21, No. 15 / August 1, 1996 Optical conveyor belts: a new scheme Research Centre, Optical Sciences Centre, Australian National University, Canberra ACT 0200, Australia with a different contrast, can be multiplexed on the same fiber. © 1996 Optical Society of America Like bright

  18. WORKSHOP ON RADIATION BELTS: MODELS & STANDARDS, BRUSSELS, 17{20 OCT., 1995 Los Alamos Geosynchronous Space Weather Data For

    E-Print Network [OSTI]

    Reeves, Geoffrey D.

    WORKSHOP ON RADIATION BELTS: MODELS & STANDARDS, BRUSSELS, 17{20 OCT., 1995 Los Alamos. Henderson, R. A. Christensen, P. S. McLachlan, and J. C. Ingraham Los Alamos National Laboratory, Mail Stop D436, Los Alamos, NM 87545, USA, reeves@lanl.gov Abstract. This paper presents an overview

  19. Integration of zircon color and zircon fission-track zonation patterns in orogenic belts: application to the

    E-Print Network [OSTI]

    Garver, John I.

    of the primary records of erosional exhuma- tion of orogenic belts is the sedimentary detritus deposited trace amounts of uranium and thorium that decay through several radiogenic processes, which change, crystal lattice transformation, and color generation. The radioactive decay of uranium and thorium

  20. Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune

    E-Print Network [OSTI]

    Harold F. Levison; Alessandro Morbidelli; Christa Van Laerhoven; Rodney Gomes; Kleomenis Tsiganis

    2007-12-04

    We explore the origin and orbital evolution of the Kuiper belt in the framework of a recent model of the dynamical evolution of the giant planets, sometimes known as the Nice model. This model is characterized by a short, but violent, instability phase, during which the planets were on large eccentricity orbits. One characteristic of this model is that the proto-planetary disk must have been truncated at roughly 30 to 35 AU so that Neptune would stop migrating at its currently observed location. As a result, the Kuiper belt would have initially been empty. In this paper we present a new dynamical mechanism which can deliver objects from the region interior to ~35 AU to the Kuiper belt without excessive inclination excitation. Assuming that the last encounter with Uranus delivered Neptune onto a low-inclination orbit with a semi-major axis of ~27 AU and an eccentricity of ~0.3, and that subsequently Neptune's eccentricity damped in ~1 My, our simulations reproduce the main observed properties of the Kuiper belt at an unprecedented level.

  1. Coupling dynamical and collisional evolution of small bodies II : Forming the Kuiper Belt, the Scattered Disk and the Oort Cloud

    E-Print Network [OSTI]

    S. Charnoz A. Morbidelli

    2006-09-29

    The Oort Cloud, the Kuiper Belt and the Scattered Disk are dynamically distinct populations of small bodies evolving in the outer regions of the Solar System. Whereas their collisional activity is now quiet, gravitational interactions with giant planets may have shaped these populations both dynamically and collisionally during their formation. Using a hybrid approach (Charnoz & Morbidelli 2003), the present paper tries to couple the primordial collisional and dynamical evolution of these three populations in a self-consistent way. A critical parameter is the primordial size-distribution. We show that the initial planetesimal size distribution that allows an effective mass depletion of the Kuiper belt by collisional grinding, would decimate also the population of comet-size bodies that end in the Oort Cloud and, in particular, in the Scattered Disk. As a consequence, the Scattered Disk and the Oort Cloud would be too anemic, by a factor 20 to 100, relative to the estimates achieved from the observation of the fluxes of long period and Jupiter family comets, respectively. For these two reservoirs to have a sufficient number of comets, the initial size distribution in the planetesimal disk had to be such that the mass depletion by collisional erosion of in the Kuiper belt was negligible. Consequently, the current mass deficit of the Kuiper belt, needs to be explained by dynamical mechanisms.

  2. RETENTION OF A PRIMORDIAL COLD CLASSICAL KUIPER BELT IN AN INSTABILITY-DRIVEN MODEL OF SOLAR SYSTEM FORMATION

    SciTech Connect (OSTI)

    Batygin, Konstantin; Brown, Michael E.; Fraser, Wesley C., E-mail: kbatygin@gps.caltech.edu [Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125 (United States)

    2011-09-01

    The cold classical population of the Kuiper Belt exhibits a wide variety of unique physical characteristics, which collectively suggest that its dynamical coherence has been maintained throughout the solar system's lifetime. Simultaneously, the retention of the cold population's relatively unexcited orbital state has remained a mystery, especially in the context of a solar system formation model, that is driven by a transient period of instability, where Neptune is temporarily eccentric. Here, we show that the cold belt can survive the instability, and its dynamical structure can be reproduced. We develop a simple analytical model for secular excitation of cold Kuiper Belt objects and show that comparatively fast apsidal precession and nodal recession of Neptune, during the eccentric phase, are essential for preservation of an unexcited state in the cold classical region. Subsequently, we confirm our results with self-consistent N-body simulations. We further show that contamination of the hot classical and scattered populations by objects of similar nature to that of cold classicals has been instrumental in shaping the vast physical diversity inherent to the Kuiper Belt.

  3. LANL LDRD-funded project: Test particle simulations of energetic ions in natural and artificial radiation belts

    SciTech Connect (OSTI)

    Cowee, Misa [Los Alamos National Laboratory; Liu, Kaijun [Los Alamos National Laboratory; Friedel, Reinhard H. [Los Alamos National Laboratory; Reeves, Geoffrey D. [Los Alamos National Laboratory

    2012-07-17

    We summarize the scientific problem and work plan for the LANL LDRD-funded project to use a test particle code to study the sudden de-trapping of inner belt protons and possible cross-L transport of debris ions after a high altitude nuclear explosion (HANE). We also discuss future application of the code for other HANE-related problems.

  4. INITIAL PLANETESIMAL SIZES AND THE SIZE DISTRIBUTION OF SMALL KUIPER BELT OBJECTS

    SciTech Connect (OSTI)

    Schlichting, Hilke E. [UCLA, Department of Earth and Space Science, 595 Charles E. Young Drive East, Los Angeles, CA 90095 (United States); Fuentes, Cesar I.; Trilling, David E., E-mail: hilke@ucla.edu [Department of Physics and Astronomy, Northern Arizona University, P.O. Box 6010, Flagstaff, AZ 86011 (United States)

    2013-08-01

    The Kuiper Belt is a remnant from the early solar system and its size distribution contains many important constraints that can be used to test models of planet formation and collisional evolution. We show, by comparing observations with theoretical models, that the observed Kuiper Belt size distribution is well matched by coagulation models, which start with an initial planetesimal population with radii of about 1 km, and subsequent collisional evolution. We find that the observed size distribution above R {approx} 30 km is primordial, i.e., it has not been modified by collisional evolution over the age of the solar system, and that the size distribution below R {approx} 30 km has been modified by collisions and that its slope is well matched by collisional evolution models that use published strength laws. We investigate in detail the resulting size distribution of bodies ranging from 0.01 km to 30 km and find that its slope changes several times as a function of radius before approaching the expected value for an equilibrium collisional cascade of material strength dominated bodies for R {approx}< 0.1 km. Compared to a single power-law size distribution that would span the whole range from 0.01 km to 30 km, we find in general a strong deficit of bodies around R {approx} 10 km and a strong excess of bodies around 2 km in radius. This deficit and excess of bodies are caused by the planetesimal size distribution left over from the runaway growth phase, which left most of the initial mass in small planetesimals while only a small fraction of the total mass is converted into large protoplanets. This excess mass in small planetesimals leaves a permanent signature in the size distribution of small bodies that is not erased after 4.5 Gyr of collisional evolution. Observations of the small Kuiper Belt Object (KBO) size distribution can therefore test if large KBOs grew as a result of runaway growth and constrained the initial planetesimal sizes. We find that results from recent KBO occultation surveys and the observed KBO size distribution can be best matched by an initial planetesimal population that contained about equal mass per logarithmic mass bin in bodies ranging from 0.4 km to 4 km in radius. We further find that we cannot match the observed KBO size distribution if most of the planetesimal mass was contained in bodies that were 10 km in radius or larger simply because their resulting size distribution cannot be sufficiently depleted over 4.5 Gyr to match observations.

  5. Accurately specifying storm-time ULF wave radial diffusion in the radiation belts

    E-Print Network [OSTI]

    Dimitrakoudis, Stavros; Balasis, Georgios; Papadimitriou, Constantinos; Anastasiadis, Anastasios; Daglis, Ioannis A

    2015-01-01

    Ultra-low frequency (ULF) waves can contribute to the transport, acceleration and loss of electrons in the radiation belts through inward and outward diffusion. However, the most appropriate parameters to use to specify the ULF wave diffusion rates are unknown. Empirical representations of diffusion coefficients often use Kp; however, specifications using ULF wave power offer an improved physics-based approach. We use 11 years of ground-based magnetometer array measurements to statistically parameterise the ULF wave power with Kp, solar wind speed, solar wind dynamic pressure and Dst. We find Kp is the best single parameter to specify the statistical ULF wave power driving radial diffusion. Significantly, remarkable high energy tails exist in the ULF wave power distributions when expressed as a function of Dst. Two parameter ULF wave power specifications using Dst as well as Kp provide a better statistical representation of storm-time radial diffusion than any single variable alone.

  6. Four Cometary Belts Associated with the Orbits of Giant Planets: A New View of the Outer Solar System's Structure Emerges from Numerical Simulations

    E-Print Network [OSTI]

    Leonid M. Ozernoy; Nick N. Gorkavyi; Tanya Taidakova

    2000-01-18

    Using numerical simulations, we examine the structure of a cometary population near a massive planet, such as a giant planet of the Solar system, starting with one-planet approximation (the Sun plus one planet). By studying the distributions of comets in semimajor axis, eccentricity, pericenter, and apocenter distances, we have revealed several interesting features in these distributions. The most remarkable ones include (i) spatial accumulation of comets near the planetary orbit (which we call the `cometary belt') and (ii) avoidance of resonant orbits by comets. Then we abandon one-planet approximation and examine as to how a cometary belt is modified when the influence of all four giant planets is taken into consideration. To this end, we simulate a stationary distribution of comets, which results from the gravitational scattering of the Kuiper belt objects on the four giant planets and accounts for the effects of mean motion resonances. Accounting for the influence of four giant planets makes the cometary belts overlapping, but nevertheless keeping almost all their basic features found in one-planet approximation. In particular, the belts maintain the gaps in the (a,e)- and (a,i)-space similar to the Kirkwood gaps in the main asteroid belt. We conclude that the large-scale structure of the Solar system is featured by the four cometary belts expected to contain 20-30 millions of scattered comets, and only a tiny fraction of them is currently visible as Jupiter-, Saturn-, etc. family comets.

  7. A PHOTOMETRIC SYSTEM FOR DETECTION OF WATER AND METHANE ICES ON KUIPER BELT OBJECTS

    SciTech Connect (OSTI)

    Trujillo, Chadwick A.; Sheppard, Scott S.; Schaller, Emily L. E-mail: sheppard@dtm.ciw.edu

    2011-04-01

    We present a new near-infrared photometric system for detection of water ice and methane ice in the solar system. The system consists of two medium-band filters in the K-band region of the near-infrared, which are sensitive to water ice and methane ice, plus continuum observations in the J band and Y band. The primary purpose of this system is to distinguish between three basic types of Kuiper Belt Objects (KBOs)-those rich in water ice, those rich in methane ice, and those with little absorbance. In this work, we present proof-of-concept observations of 51 KBOs using our filter system, 21 of which have never been observed in the near-infrared spectroscopically. We show that our custom photometric system is consistent with previous spectroscopic observations while reducing telescope observing time by a factor of {approx}3. We use our filters to identify Haumea collisional family members, which are thought to be collisional remnants of a much larger body and are characterized by large fractions of water ice on their surfaces. We add 2009 YE{sub 7} to the Haumea collisional family based on our water ice band observations (J - H{sub 2}O = -1.03 {+-} 0.27) which indicate a high amount of water ice absorption, our calculated proper orbital elements, and the neutral optical colors we measured, V - R = 0.38 {+-} 0.04, which are all consistent with the rest of the Haumea family. We identify several objects dynamically similar to Haumea as being distinct from the Haumea family as they do not have water ice on their surfaces. In addition, we find that only the largest KBOs have methane ice, and Haumea itself has significantly less water ice absorption than the smaller Haumea family members. We find no evidence for other families in the Kuiper Belt.

  8. NEPTUNE'S WILD DAYS: CONSTRAINTS FROM THE ECCENTRICITY DISTRIBUTION OF THE CLASSICAL KUIPER BELT

    SciTech Connect (OSTI)

    Dawson, Rebekah I.; Murray-Clay, Ruth, E-mail: rdawson@cfa.harvard.edu [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-51, Cambridge, MA 02138 (United States)

    2012-05-01

    Neptune's dynamical history shaped the current orbits of Kuiper Belt objects (KBOs), leaving clues to the planet's orbital evolution. In the 'classical' region, a population of dynamically 'hot' high-inclination KBOs overlies a flat 'cold' population with distinct physical properties. Simulations of qualitatively different histories for Neptune, including smooth migration on a circular orbit or scattering by other planets to a high eccentricity, have not simultaneously produced both populations. We explore a general Kuiper Belt assembly model that forms hot classical KBOs interior to Neptune and delivers them to the classical region, where the cold population forms in situ. First, we present evidence that the cold population is confined to eccentricities well below the limit dictated by long-term survival. Therefore, Neptune must deliver hot KBOs into the long-term survival region without excessively exciting the eccentricities of the cold population. Imposing this constraint, we explore the parameter space of Neptune's eccentricity and eccentricity damping, migration, and apsidal precession. We rule out much of parameter space, except where Neptune is scattered to a moderately eccentric orbit (e > 0.15) and subsequently migrates a distance {Delta}a{sub N} = 1-6 AU. Neptune's moderate eccentricity must either damp quickly or be accompanied by fast apsidal precession. We find that Neptune's high eccentricity alone does not generate a chaotic sea in the classical region. Chaos can result from Neptune's interactions with Uranus, exciting the cold KBOs and placing additional constraints. Finally, we discuss how to interpret our constraints in the context of the full, complex dynamical history of the solar system.

  9. OPTICAL AND DYNAMICAL CHARACTERIZATION OF COMET-LIKE MAIN-BELT ASTEROID (596) SCHEILA

    SciTech Connect (OSTI)

    Hsieh, Henry H.; Yang Bin; Haghighipour, Nader, E-mail: hsieh@ifa.hawaii.edu, E-mail: yangbin@ifa.hawaii.edu, E-mail: nader@ifa.hawaii.edu [Institute for Astronomy, Univ. of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States)

    2012-01-01

    We present observations and a dynamical analysis of the comet-like main-belt object, (596) Scheila. V-band photometry obtained on UT 2010 December 12 indicates that Scheila's dust cloud has a scattering cross-section {approx}1.4 times larger than that of the nucleus, corresponding to a dust mass of M{sub d} {approx} 3 Multiplication-Sign 10{sup 7} kg. V-R color measurements indicate that both the nucleus and dust are redder than the Sun, with no significant color differences between the dust cloud's northern and southern plumes. We also undertake an ultimately unsuccessful search for CN emission, where we find CN and H{sub 2}O production rates of Q{sub CN} < 9 Multiplication-Sign 10{sup 23} s{sup -1} and Q{sub H{sub 2O}}<10{sup 27} s{sup -1}. Numerical simulations indicate that Scheila is dynamically stable for >100 Myr, suggesting that it is likely native to its current location. We also find that it does not belong to a dynamical asteroid family of any significance. We consider sublimation-driven scenarios that could produce the appearance of multiple plumes of dust emission, but reject them as being physically implausible. Instead, we concur with previous studies that the unusual morphology of Scheila's dust cloud is most simply explained by a single oblique impact, meaning that this object is likely not a main-belt comet but is instead the second disrupted asteroid after P/2010 A2 (LINEAR) to be discovered.

  10. Preparing for Transfer Biological Engineering

    E-Print Network [OSTI]

    Walter, M.Todd

    Preparing for Transfer Majors: Biological Engineering Chemical Engineering Civil Engineering Computer Science Electrical & Computer Engineering Engineering Physics Environmental Engineering Information Science, Systems, & Technology Materials Science & Engineering Mechanical Engineering Operations

  11. Preparing for Transfer Biological Engineering

    E-Print Network [OSTI]

    Walter, M.Todd

    Preparing for Transfer Majors: Biological Engineering Biomedical Engineering* Chemical Engineering Civil Engineering Computer Science Electrical & Computer Engineering Engineering Physics Environmental Engineering Information Science, Systems, & Technology Materials Science & Engineering Mechanical Engineering

  12. Method for preparation of polysilanes

    DOE Patents [OSTI]

    Zeigler, John M. (2208 Lester Dr., NE, Albuquerque, NM 87112)

    1991-01-01

    High molecular weight polysilanes are prepared using highly non-chain-transferring solvents. Certain alloys of sodium can also be used to advantage with such solvents. The high molecular weights are achievable even in the commercially preferred "normal" addition procedure.

  13. HYDRAULIC CEMENT PREPARATION FROM LURGI SPENT SHALE

    E-Print Network [OSTI]

    Mehta, P.K.

    2013-01-01

    P. , "Investigations on hydraulic cement from spent oilCO, April 16-18, 1980 HYDRAULIC CEMENT PREPARATION FROMUniversity of California. HYDRAULIC CEMENT PREPARATION FROM

  14. On the possibility to use semiconductive hybrid pixel detectors for study of radiation belt of the Earth

    E-Print Network [OSTI]

    Guskov, A; Smolyanskiy, P; Zhemchugov, A

    2015-01-01

    The scientific apparatus "Gamma-400" designed for study of hadron and electromagnetic components of cosmic rays will be launched to an elliptic orbit with the apogee of about 300 000 km and the perigee of about 500 km. Such a configuration of the orbit allows it to cross periodically the radiation belt and the outer part of magnetosphere. We discuss the possibility to use hybrid pixel detecters based on the Timepix chip and semiconductive sensors on board the "Gamma-400" apparatus. Due to high granularity of the sensor (pixel size is 55 $mu$m) and possibility to measure independently an energy deposition in each pixel, such compact and lightweight detector could be a unique instrument for study of spatial, energy and time structure of electron and proton components of the radiation belt.

  15. THE DENSITY OF MID-SIZED KUIPER BELT OBJECT 2002 UX25 AND THE FORMATION OF THE DWARF PLANETS

    SciTech Connect (OSTI)

    Brown, M. E., E-mail: mbrown@caltech.edu [Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125 (United States)

    2013-12-01

    The formation of the largest objects in the Kuiper belt, with measured densities of ?1.5 g cm{sup –3} and higher, from the coagulation of small bodies, with measured densities below 1 g cm{sup –3}, is difficult to explain without invoking significant porosity in the smallest objects. If such porosity does occur, measured densities should begin to increase at the size at which significant porosity is no longer supported. Among the asteroids, this transition occurs for diameters larger than ?350 km. In the Kuiper belt, no density measurements have been made between ?350 km and ?850 km, the diameter range where porosities might first begin to drop. Objects in this range could provide key tests of the rock fraction of small Kuiper belt objects (KBOs). Here we report the orbital characterization, mass, and density determination of the 2002 UX25 system in the Kuiper belt. For this object, with a diameter of ?650 km, we find a density of 0.82 ± 0.11 g cm{sup –3}, making it the largest solid known object in the solar system with a measured density below that of pure water ice. We argue that the porosity of this object is unlikely to be above ?20%, suggesting a low rock fraction. If the currently measured densities of KBOs are a fair representation of the sample as a whole, creating ?1000 km and larger KBOs with rock mass fractions of 70% and higher from coagulation of small objects with rock fractions as low as those inferred from 2002 UX25 is difficult.

  16. Twin-belt continuous caster with containment and cooling of the exiting cast product for enabling high-speed casting of molten-center product

    DOE Patents [OSTI]

    Dykes, Charles D. (303 Shore Rd., Milton, VT); Daniel, Sabah S. (303 Shore Rd., Pittsburgh, PA); Wood, J. F. Barry (303 Shore Rd., Burlington, VT 05401)

    1990-02-20

    In continuously casting molten metal into cast product by a twin-belt machine, it is desirable to achieve dramatic increases in speed (linear feet per minute) at which cast product exits the machine, particularly in installations where steel cast product is intended to feed a downstream regular rolling mill (as distinct from a planetary mill) operating in tandem with the twin-belt caster. Such high-speed casting produces product with a relatively thin shell and molten interior, and the shell tends to bulge outwardly due to metallostatic head pressure of the molten center. A number of cooperative features enable high-speed, twin-belt casting: (1) Each casting belt is slidably supported adjacent to the caster exit pulley for bulge control and enhanced cooling of cast product. (2) Lateral skew steering of each belt provides an effective increase in moving mold length plus a continuity of heat transfer not obtained with prior art belt steering apparatus. (3) The exiting slab is contained and supported downstream from the casting machine to prevent bulging of the shell of the cast product, and (4) spray cooling is incorporated in the exit containment apparatus for secondary cooling of cast product.

  17. Warm exo-Zodi from cool exo-Kuiper belts: the significance of P-R drag and the inference of intervening planets

    E-Print Network [OSTI]

    Kennedy, Grant M

    2015-01-01

    Poynting-Robertson drag has been considered an ineffective mechanism for delivering dust to regions interior to the cool Kuiper belt analogues seen around other Sun-like stars. This conclusion is however based on the very large contrast in dust optical depth between the parent belt and the interior regions that results from the dominance of collisions over drag in systems with detectable cool belts. Here, we show that the levels of habitable zone dust arising from detectable Kuiper belt analogues can be tens to a few hundreds of times greater than the optical depth in the Solar Zodiacal cloud. Dust enhancements of more than a few tens of `zodi' are expected to hinder future Earth-imaging missions, but relatively few undetectable Kuiper belts result in such levels, particularly around stars older than a few Gyr. Thus, current mid to far-IR photometric surveys have already identified most of the 20-25% of nearby stars where P-R drag from outer belts could seriously impact Earth-imaging. The LBTI should easily d...

  18. HIGH-ALBEDO C-COMPLEX ASTEROIDS IN THE OUTER MAIN BELT: THE NEAR-INFRARED SPECTRA

    SciTech Connect (OSTI)

    Kasuga, Toshihiro [Public Relations Center, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Usui, Fumihiko; Hasegawa, Sunao [Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara 252-5210 (Japan); Ootsubo, Takafumi [Astronomical Institute, Tohoku University, 6-3 Aoba, Aramaki, Aoba-ku, Sendai 980-8578 (Japan); Kuroda, Daisuke, E-mail: toshi.kasuga@nao.ac.jp [Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, 3037-5 Honjo, Kamogata, Asakuchi, Okayama 719-0232 (Japan)

    2013-07-01

    Primitive, outer-belt asteroids are generally of low albedo, reflecting carbonaceous compositions like those of CI and CM meteorites. However, a few outer-belt asteroids having high albedos are known, suggesting the presence of unusually reflective surface minerals or, conceivably, even exposed water ice. Here, we present near-infrared (1.1-2.5 {mu}m) spectra of four outer-belt C-complex asteroids with albedos {>=}0.1. We find no absorption features characteristic of water ice (near 1.5 and 2.0 {mu}m) in the objects. Intimate mixture models set limits to the water ice by weight {<=}2%. Asteroids (723) Hammonia and (936) Kunigunde are featureless and have (60%-95%) amorphous Mg pyroxenes that might explain the high albedos. Asteroid (1276) Ucclia also shows a featureless reflection spectrum with (50%-60%) amorphous Mg pyroxenes. Asteroid (1576) Fabiola shows a possible weak, broad absorption band (1.5-2.1 {mu}m). The feature can be reproduced by (80%) amorphous Mg pyroxenes or orthopyroxene (crystalline silicate), either of which is likely to cause its high albedo. We discuss the origin of high-albedo components in primitive asteroids.

  19. 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)

    2011-09-15

    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.

  20. Gold deposits in the late Archaean Nzega-Igunga greenstone belt, central plateau of tanzania

    SciTech Connect (OSTI)

    Feiss, P.G.; Siyomana, S.

    1985-01-01

    2.2 m oz of gold have been produced, since 1935, from late Archaean (2480-2740 Ma) greenstone belts of the Central Plateau, Tanzania. North and east of Nzega (4/sup 0/12'S, 3/sup 0/11'E), 18% of the exposed basement, mainly Dodoman schists and granites, consists of metavolcanics and metasediments of the Nyanzian and Kavirondian Series. Four styles of mineralization are observed. 1. Stratabound quartz-gold veins with minor sulfides. Host rocks are quartz porphyry, banded iron formation (BIF), magnetite quartzite, and dense, cherty jasperite at the Sekenke and Canuck mines. The Canuck veins are on strike from BIF's in quartz-eye porphyry of the Igusule Hills. 2. Stratabound, disseminated gold in coarse-grained, crowded feldspar porphyry with lithic fragments and minor pyrite. At Bulangamilwa, the porphyry is conformable with Nyanzian-aged submarine (.) greenstone, volcanic sediment, felsic volcanics, and sericite phyllite. The deposits are on strike with BIF of the Wella Hills, which contains massive sulfide with up to 15% Pb+Zn. 3. Disseminated gold in quartz-albite metasomes in Nyanzian greenstones. At Kirondatal, alteration is associated with alaskites and feldspar porphyry dikes traceable several hundred meters into post-Dodoman diorite porphyry. Gold is with pyrite, arsenopyrite, pyrrhotite, minor chalcopyrite, and sphalerite as well as tourmalinite and silica-cemented breccias. 4. Basal Kavirondian placers in metaconglomerates containing cobbles and boulders of Dodoman and Nyanzian rocks several hundred meters up-section from the stratabound, disseminated mineralization at Bulangamilwa.

  1. A Search for Subkilometer-sized Ordinary Chondrite Like Asteroids in the Main-Belt

    E-Print Network [OSTI]

    Lin, H W; Chen, Y T; Ip, W H; Chang, C K

    2015-01-01

    The size-dependent effects of asteroids on surface regolith and collisional lifetimes suggest that small asteroids are younger than large asteroids. In this study, we performed multicolor main-belt asteroid (MBA) survey by Subaru telescope/Suprime-Cam to search for subkilometer-sized ordinary chondrite (Q-type) like MBAs. The total survey area was 1.5 deg^2 near ecliptic plane and close to the opposition. We detected 150 MBAs with 4 bands (B, V , R, I) in this survey. The range of absolute magnitude of detected asteroids was between 13 and 22 magnitude, which is equivalent to the size range of kilometer to sub-kilometer diameter in MBAs. From this observation, 75 of 150 MBAs with color uncertainty less than 0.1 were used in the spectral type analysis, and two possible Q-type aster- oids were detected. This mean that the Q-type to S-type ratio in MBAs is < 0.05. Meanwhile, the Q/S ratio in near Earth asteroids (NEAs) has been estimated to be 0.5 to 2 (Binzel et al., 2004; Dandy et al., 2003). Therefore, Q-t...

  2. Lumpy AdS$\\bf{_5\\times}$ S$\\bf{^5}$ Black Holes and Black Belts

    E-Print Network [OSTI]

    Oscar J. C. Dias; Jorge E. Santos; Benson Way

    2015-01-26

    Sufficiently small Schwarzschild black holes in global AdS$_5\\times$S$^5$ are Gregory-Laflamme unstable. We construct new families of black hole solutions that bifurcate from the onset of this instability and break the full SO$(6)$ symmetry group of the S$^5$ down to SO$(5)$. These new "lumpy" solutions are labelled by the harmonics $\\ell$. We find evidence that the $\\ell = 1$ branch never dominates the microcanonical/canonical ensembles and connects through a topology-changing merger to a localised black hole solution with S$^8$ topology. We argue that these S$^8$ black holes should become the dominant phase in the microcanonical ensemble for small enough energies, and that the transition to Schwarzschild black holes is first order. Furthermore, we find two branches of solutions with $\\ell = 2$. We expect one of these branches to connect to a solution containing two localised black holes, while the other branch connects to a black hole solution with horizon topology $\\mathrm S^4\\times\\mathrm S^4$ which we call a "black belt".

  3. The JCMT Gould Belt Survey: A Quantitative Comparison Between SCUBA-2 Data Reduction Methods

    E-Print Network [OSTI]

    Mairs, S; Kirk, H; Graves, S; Buckle, J; Beaulieu, S F; Berry, D S; Broekhoven-Fiene, H; Currie, M J; Fich, M; Hatchell, J; Jenness, T; Mottram, J C; Nutter, D; Pattle, K; Pineda, J E; Salji, C; Di Francesco, J; Hogerheijde, M R; Ward-Thompson, D

    2015-01-01

    Performing ground-based submillimetre observations is a difficult task as the measurements are subject to absorption and emission from water vapour in the Earth's atmosphere and time variation in weather and instrument stability. Removing these features and other artifacts from the data is a vital process which affects the characteristics of the recovered astronomical structure we seek to study. In this paper, we explore two data reduction methods for data taken with the Submillimetre Common-User Bolometer Array-2 (SCUBA-2) at the James Clerk Maxwell Telescope (JCMT). The JCMT Legacy Reduction 1 (JCMT LR1) and The Gould Belt Legacy Survey Legacy Release 1 (GBS LR1) reduction both use the same software, Starlink, but differ in their choice of data reduction parameters. We find that the JCMT LR1 reduction is suitable for determining whether or not compact emission is present in a given region and the GBS LR1 reduction is tuned in a robust way to uncover more extended emission, which better serves more in-depth ...

  4. Precise Distances for Main-Belt Asteroids in Only Two Nights

    E-Print Network [OSTI]

    Heinze, Aren N

    2015-01-01

    We present a method for calculating precise distances to asteroids using only two nights of data from a single location --- far too little for an orbit --- by exploiting the angular reflex motion of the asteroids due to Earth's axial rotation. We refer to this as the rotational reflex velocity method. While the concept is simple and well-known, it has not been previously exploited for surveys of main-belt asteroids. We offer a mathematical development, estimates of the errors of the approximation, and a demonstration using a sample of 197 asteroids observed for two nights with a small, 0.9-meter telescope. This demonstration used digital tracking to enhance detection sensitivity for faint asteroids, but our distance determination works with any detection method. Forty-eight asteroids in our sample had known orbits prior to our observations, and for these we demonstrate a mean fractional error of only 1.6% between the distances we calculate and those given in ephemerides from the Minor Planet Center. In contra...

  5. THE DUST ENVIRONMENT OF MAIN-BELT COMET P/2012 T1 (PANSTARRS)

    SciTech Connect (OSTI)

    Moreno, F.; Pozuelos, F. [Instituto de Astrofisica de Andalucia, CSIC, Glorieta de la Astronomia s/n, E-18008 Granada (Spain); Cabrera-Lavers, A.; Vaduvescu, O.; Licandro, J., E-mail: fernando@iaa.es [Instituto de Astrofisica de Canarias, c/Via Lactea s/n, E-38200 La Laguna, Tenerife (Spain)

    2013-06-20

    The Main-Belt Comet P/2012 T1 (PANSTARRS) has been imaged using the 10.4 m Gran Telescopio Canarias and the 4.2 m William Herschel Telescope at six epochs in the period from 2012 November to 2013 February, with the aim of monitoring its dust environment. The dust tails' brightness and morphology are best interpreted in terms of a model of sustained dust emission spanning four to six months. The total dust mass ejected is estimated at {approx}6-25 Multiplication-Sign 10{sup 6} kg. We assume a time-independent power-law size distribution function, with particles in the micrometer to centimeter size range. Based on the quality of the fits to the isophote fields, an anisotropic emission pattern is favored against an isotropic one, in which the particle ejection is concentrated toward high latitudes ({+-}45 Degree-Sign to {+-}90 Degree-Sign ) in a high-obliquity object (I = 80 Degree-Sign ). This seasonally driven ejection behavior, along with the modeled particle ejection velocities, are in remarkable agreement to those we found for P/2010 R2 (La Sagra).

  6. ON A POSSIBLE SIZE/COLOR RELATIONSHIP IN THE KUIPER BELT

    SciTech Connect (OSTI)

    Pike, R. E.; Kavelaars, J. J., E-mail: repike@uvic.ca [Department of Physics and Astronomy, University of Victoria, Victoria, BC V8W 3P6 (Canada)

    2013-10-01

    Color measurements and albedo distributions introduce non-intuitive observational biases in size-color relationships among Kuiper Belt Objects (KBOs) that cannot be disentangled without a well characterized sample population with systematic photometry. Peixinho et al. report that the form of the KBO color distribution varies with absolute magnitude, H. However, Tegler et al. find that KBO color distributions are a property of object classification. We construct synthetic models of observed KBO colors based on two B-R color distribution scenarios: color distribution dependent on H magnitude (H-Model) and color distribution based on object classification (Class-Model). These synthetic B-R color distributions were modified to account for observational flux biases. We compare our synthetic B-R distributions to the observed ''Hot'' and ''Cold'' detected objects from the Canada-France Ecliptic Plane Survey and the Meudon Multicolor Survey. For both surveys, the Hot population color distribution rejects the H-Model, but is well described by the Class-Model. The Cold objects reject the H-Model, but the Class-Model (while not statistically rejected) also does not provide a compelling match for data. Although we formally reject models where the structure of the color distribution is a strong function of H magnitude, we also do not find that a simple dependence of color distribution on orbit classification is sufficient to describe the color distribution of classical KBOs.

  7. The JCMT Gould Belt Survey: A First Look at Dense Cores in Orion B

    E-Print Network [OSTI]

    Kirk, H; Johnstone, D; Duarte-Cabral, A; Sadavoy, S; Hatchell, J; Mottram, J C; Buckle, J; Berry, D S; Broekhoven-Fiene, H; Currie, M J; Fich, M; Jenness, T; Nutter, D; Pattle, K; Pineda, J E; Quinn, C; Salji, C; Tisi, S; Hogerheijde, M R; Ward-Thompson, D; Bastien, P; Bresnahan, D; Butner, H; Chen, M; Chrysostomou, A; Coude, S; Davis, C J; Drabek-Maunder, E; Fiege, J; Friberg, P; Friesen, R; Fuller, G A; Graves, S; Greaves, J; Gregson, J; Holland, W; Joncas, G; Kirk, J M; Knee, L B G; Mairs, S; Marsh, K; Matthews, B C; Moriarty-Schieven, G; Mowat, C; Rawlings, J; Richer, J; Robertson, D; Rosolowsky, E; Rumble, D; Thomas, H; Tothill, N; Viti, S; White, G J; Wouterloot, J; Yates, J; Zhu, M

    2015-01-01

    We present a first look at the SCUBA-2 observations of three sub-regions of the Orion B molecular cloud: LDN 1622, NGC 2023/2024, and NGC 2068/2071, from the JCMT Gould Belt Legacy Survey. We identify 29, 564, and 322 dense cores in L1622, NGC 2023/2024, and NGC 2068/2071 respectively, using the SCUBA-2 850 micron map, and present their basic properties, including their peak fluxes, total fluxes, and sizes, and an estimate of the corresponding 450 micron peak fluxes and total fluxes, using the FellWalker source extraction algorithm. Assuming a constant temperature of 20 K, the starless dense cores have a mass function similar to that found in previous dense core analyses, with a Salpeter-like slope at the high-mass end. The majority of cores appear stable to gravitational collapse when considering only thermal pressure; indeed, most of the cores which have masses above the thermal Jeans mass are already associated with at least one protostar. At higher cloud column densities, above 1-2 x 10^23 cm^-2, most of ...

  8. The JCMT Gould Belt Survey: SCUBA-2 observations of circumstellar disks in L 1495

    E-Print Network [OSTI]

    Buckle, J V; Greaves, J; Richer, J S; Matthews, B C; Johnstone, D; Kirk, H; Beaulieu, S F; Berry, D S; Broekhoven-Fiene, H; Currie, M J; Fich, M; Hatchell, J; Jenness, T; Mottram, J C; Nutter, D; Pattle, K; Pineda, J E; Salji, C; Tisi, S; Di Francesco, J; Hogerheijde, M R; Ward-Thompson, D; Bastien, P; Butner, H; Chen, M; Chrysostomou, A; Coude, S; Davis, C J; Duarte-Cabral, A; Friberg, P; Friesen, R; Fuller, G A; Graves, S; Gregson, J; Holland, W; Joncas, G; Kirk, J M; Knee, L B G; Mairs, S; Marsh, K; Moriarty-Schieven, G; Rawlings, J; Rosolowsky, E; Rumble, D; Sadavoy, S; Thomas, H; Tothill, N; Viti, S; White, G J; Wilson, C D; Wouterloot, J; Yates, J; Zhu, M

    2015-01-01

    We present 850$\\mu$m and 450$\\mu$m data from the JCMT Gould Belt Survey obtained with SCUBA-2 and characterise the dust attributes of Class I, Class II and Class III disk sources in L1495. We detect 23% of the sample at both wavelengths, with the detection rate decreasing through the Classes from I--III. The median disk mask is 1.6$\\times 10^{-3}$M$_{\\odot}$, and only 7% of Class II sources have disk masses larger than 20 Jupiter masses. We detect a higher proportion of disks towards sources with stellar hosts of spectral type K than spectral type M. Class II disks with single stellar hosts of spectral type K have higher masses than those of spectral type M, supporting the hypothesis that higher mass stars have more massive disks. Variations in disk masses calculated at the two wavelengths suggests there may be differences in dust opacity and/or dust temperature between disks with hosts of spectral types K to those with spectral type M.

  9. A long-lived relativistic electron storage ring embedded in Earth's Outer Van Allen belt

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

    Baker, D. N.; Kanekal, S. G.; Hoxie, V. C.; Henderson, M. G.; Li, X.; Spence, H. E.; Elkington, S. R.; Friedel, R. H. W.; Goldstein, J.; Hudson, M. K.; et al

    2013-02-28

    Since their discovery over 50 years ago, the Earth’s Van Allen radiation belts are thought to consist of two distinct zones of trapped, highly energetic charged particles. The outer zone is comprised predominantly of mega-electron volt (MeV) electrons that wax and wane in intensity on time scales ranging from hours to days depending primarily on external forcing by the solar wind. Thus, the spatially separated inner zone is comprised of commingled high-energy electrons and very energetic positive ions (mostly protons), the latter being stable in intensity levels over years to decades. In situ energy-specific and temporally resolved spacecraft observations revealmore »an isolated third ring, or torus, of high-energy (E > 2 MeV) electrons that formed on 2 September 2012 and persisted largely unchanged in the geocentric radial range of 3.0 to ~3.5 Earth radii for over four weeks before being disrupted (and virtually annihilated) by a powerful interplanetary shock wave passage.« less

  10. Simulating the Heterogeneity in Braided Channel Belt Deposits: 2. Examples of Results and Comparison to Natural Deposits

    SciTech Connect (OSTI)

    Guin, Arijit; Ramanathan, Ramya; Ritzi, Robert W.; Dominic, David F.; Lunt, Ian A.; Scheibe, Timothy D.; Freedman, Vicky L.

    2010-04-29

    In Part 1 of this series we presented a methodology and a code for modeling the hierarchical sedimentary architecture in braided channel belt deposits. Here, in Part 2, the code was used to create a digital model of this architecture, and the corresponding spatial distribution of permeability. The simulated architecture was compared to the real stratal architecture observed in an abandoned channel belt of the Sagavanirktok River, Alaska by Lunt et al. (2004). The comparisons included assessments of similarity which were both qualitative and quantitative. From the qualitative comparisons we conclude that a synthetic deposit created by the code has unit types, at each level, with a geometry which is generally consistent with the geometry of unit types observed in the field. The digital unit types would generally be recognized as representing their counterparts in nature, including cross stratasets, lobate and scroll bar deposits, channel fills, etc. Furthermore, the synthetic deposit has a hierarchical spatial relationship among these units which represents how the unit types are observed in field exposures and in geophysical images. In quantitative comparisons the proportions and the length, width, and height of unit types at different scales, across all levels of the stratal hierarchy compare well between the digital and the natural deposits. A number of important attributes of the channel belt model were shown to be influenced by more than one level within the hierarchy of stratal architecture. First, the high-permeability open-framework gravels percolated at all levels and thus formed preferential flow pathways. Open framework gravels are indeed known to form preferential flow pathways in natural channel belt deposits. The nature of a percolating cluster changed across different levels of the hierarchy of stratal architecture. As a result of this geologic structure, the percolation occurs at proportions of open-framework gravels below the theoretical percolation threshold for random infinite media. Second, when the channel belt model was populated with permeability distributions by lowest-level unit type, the composite permeability semivariogram contained structures that were identifiable at more than one scale, and each of these structures could be directly linked to unit types of different scales existing at different levels within the hierarchy of strata. These collective results are encouraging with respect to our goal that this model be relevant as a base case in future studies for testing ideas in research addressing the upscaling problem in aquifers and reservoirs with multi-scale heterogeneity.

  11. Preparation of RCRA contingency plans

    SciTech Connect (OSTI)

    Not Available

    1992-07-01

    The purpose of this guidance is to assist Department of Energy (DOE) field personnel in the preparation of Resource Conservation and Recovery Act (RCRA) contingency plans as set forth in 40 CFR 264/265 Subpart D and 270.42. The guidance will assist personnel in evaluating and ensuring facility compliance with the contingency plan requirements.

  12. Preparation of gas selective membranes

    DOE Patents [OSTI]

    Kulprathipanja, Santi (Hoffman Estates, IL); Kulkarni, Sudhir S. (Hoffman Estates, IL); Funk, Edward W. (Highland Park, IL)

    1988-01-01

    Gas separation membranes which possess improved characteristics as exemplified by selectivity and flux may be prepared by coating a porous organic polymer support with a solution or emulsion of a plasticizer and an organic polymer, said coating being effected at subatmospheric pressures in order to increase the penetration depth of the coating material.

  13. JOURNAL AUTHORS SURVEY Prepared by

    E-Print Network [OSTI]

    Stevenson, Paul

    JISC/OSI JOURNAL AUTHORS SURVEY Report Prepared by Key Perspectives Ltd 48 Old Coach Road, Playing behind its development 4 2.2 Models and definitions of open access 8 2.2.1 Open access journals 8 2 4.1 Respondent profiles 18 4.2 Awareness of open access journals 18 4.2.1 Extent and longevity

  14. Photochemical preparation of plutonium pentafluoride

    DOE Patents [OSTI]

    Rabideau, Sherman W. (Los Alamos, NM); Campbell, George M. (Los Alamos, NM)

    1987-01-01

    The novel compound plutonium pentafluoride may be prepared by the photodissociation of gaseous plutonium hexafluoride. It is a white solid of low vapor pressure, which consists predominantly of a face-centered cubic structure with a.sub.o =4.2709.+-.0.0005 .ANG..

  15. Preparation of asymmetric porous materials

    DOE Patents [OSTI]

    Coker, Eric N. (Albuquerque, NM)

    2012-08-07

    A method for preparing an asymmetric porous material by depositing a porous material film on a flexible substrate, and applying an anisotropic stress to the porous media on the flexible substrate, where the anisotropic stress results from a stress such as an applied mechanical force, a thermal gradient, and an applied voltage, to form an asymmetric porous material.

  16. Arduino Sustainability Project Prepared for

    E-Print Network [OSTI]

    Kachroo, Pushkin

    Arduino Sustainability Project Prepared for: Dr. Pushkin Kachroo EE 290 UNLV Christian Calvo 2009 by the Arduino microcontroller to satisfy the theme of sustainability. The device I decided to construct is determined by the LDR. The LDR output signal is fed into an analog input of the Arduino. The value is read

  17. Guide to Petrography Specimen Preparation

    E-Print Network [OSTI]

    Henderson, Gideon

    I Microscopic Examination I Image Analysis & Capture #12;In 1849 when Henry Sorby, the father of pet's technologies help deliver the fullest product offering for all applications. Together with our technical in the case of preparing thin sections) · Expose the surface of interest Historically, the sectioning process

  18. Agile machining and inspection thrust area team-on-machine probing / compatibility assessment of Parametric Technology Corporation (PTC) pro/CMM DMIS with Zeiss DMISEngine.

    SciTech Connect (OSTI)

    Wade, James Rokwel; Tomlinson, Kurt; Bryce, Edwin Anthony

    2008-09-01

    The charter goal of the Agile Machining and Inspection Thrust Area Team is to identify technical requirements, within the nuclear weapons complex (NWC), for Agile Machining and Inspection capabilities. During FY 2008, the team identified Parametric Technology Corporation (PTC) Pro/CMM as a software tool for use in off-line programming of probing routines--used for measurement--for machining and turning centers. The probing routine would be used for in-process verification of part geometry. The same Pro/CMM program used on the machine tool could also be employed for program validation / part verification using a coordinate measuring machine (CMM). Funding was provided to determine the compatibility of the Pro/CMM probing program with CMM software (Zeiss DMISEngine).

  19. ACCEPTED MANUSCRIPT Fold interaction and wavelength selection

    E-Print Network [OSTI]

    Kaus, Boris

    with the Fars region of the Zagros fold-and-thrust belt including a large range of fold aspect ratio, such as the Makran, appear to be dominated by thrusting, whereas others such as the Simply Folded Belt at Zagros is active which amplifies sufficiently fast. In the Zagros Simply Folded Belt, they argued that weak

  20. Survey and discussion of models applicable to the transport and fate thrust area of the Department of Energy Chemical and Biological Nonproliferation Program

    SciTech Connect (OSTI)

    1997-09-01

    The availability and easy production of toxic chemical and biological agents by domestic and international terrorists pose a serious threat to US national security, especially to civilian populations in and around urban areas. To address this threat, the Department of Energy (DOE) has established the Chemical and Biological Nonproliferation Program (CBNP) with the goal of focusing the DOE`s technical resources and expertise on capabilities to deny, deter, mitigate and respond to clandestine releases of chemical and biological agents. With the intent to build on DOE core competencies, the DOE has established six technology thrust areas within the CBNP Program: Biological Information Resources; Point Sensor Systems; Stand-off Detection; Transport and Fate; Decontamination; and Systems Analysis and Integration. The purpose of the Transport and Fate Thrust is to accurately predict the dispersion, concentration and ultimate fate of chemical and biological agents released into the urban and suburban environments and has two major goals: (1) to develop an integrated and validated state-of-the-art atmospheric transport and fate modeling capability for chemical and biological agent releases within the complex urban environment from the regional scale down to building and subway interiors, and (2) to apply this modeling capability in a broad range of simulation case studies of chemical and biological agent release scenarios in suburban, urban and confined (buildings and subways) environments and provide analysis for the incident response user community. Sections of this report discuss subway transport and fate models; buildings interior transport and fate modeling; models for flow and transport around buildings; and local-regional meteorology and dispersion models.

  1. Prepared

    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: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefield Municipal Gas &SCE-SessionsSouthReport for the t-) S/,,5 'a C O M1 the RFSOGorPLEASE RETURN

  2. Performance of integrated retainer rings in silicon micro-turbines with thrust style micro-ball This article has been downloaded from IOPscience. Please scroll down to see the full text article.

    E-Print Network [OSTI]

    Ghodssi, Reza

    silicon rotary micromachines were demonstrated [1]. These devices had simple journal or thrust bearings as these allow replenishment of the lubricant. In parallel with the above, levitation schemes based on electrostatic, magnetic or hydrostatic forces have been developed [6­9]. These are highly effective but require

  3. MEASURING THE ABUNDANCE OF SUB-KILOMETER-SIZED KUIPER BELT OBJECTS USING STELLAR OCCULTATIONS

    SciTech Connect (OSTI)

    Schlichting, Hilke E. [Department of Earth and Space Science, UCLA, 595 Charles East Young Drive East, Los Angeles, CA 90095 (United States); Ofek, Eran O.; Gal-Yam, Avishay [Faculty of Physics, Weizmann Institute of Science, P.O. Box 26, Rehovot 76100 (Israel); Sari, Re'em [Racah Institute of Physics, Hebrew University, Jerusalem 91904 (Israel); Nelan, Edmund P.; Livio, Mario [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Wenz, Michael [Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771 (United States); Muirhead, Philip [Department of Astronomy, California Institute of Technology, MC 130-33, Pasadena, CA 91125 (United States); Javanfar, Nikta, E-mail: hilke@ucla.edu [Department of Physics, Physics Engineering and Astronomy, Queen's University, 99 University Avenue, Kingston, Ontario K7L 3N6 (Canada)

    2012-12-20

    We present here the analysis of about 19,500 new star hours of low ecliptic latitude observations (|b| {<=} 20 Degree-Sign ) obtained by the Hubble Space Telescope's Fine Guidance Sensors over a time span of more than nine years, which is in addition to the {approx}12, 000 star hours previously analyzed by Schlichting et al. Our search for stellar occultations by small Kuiper Belt Objects (KBOs) yielded one new candidate event corresponding to a body with a 530 {+-} 70 m radius at a distance of about 40 AU. Using bootstrap simulations, we estimate a probability of Almost-Equal-To 5% that this event is due to random statistical fluctuations within the new data set. Combining this new event with the single KBO occultation reported by Schlichting et al. we arrive at the following results: (1) the ecliptic latitudes of 6. Degree-Sign 6 and 14. Degree-Sign 4 of the two events are consistent with the observed inclination distribution of larger, 100-km-sized KBOs. (2) Assuming that small, sub-kilometer-sized KBOs have the same ecliptic latitude distribution as their larger counterparts, we find an ecliptic surface density of KBOs with radii larger than 250 m of N(r > 250 m) = 1.1{sup +1.5}{sub -0.7} Multiplication-Sign 10{sup 7} deg{sup -2}; if sub-kilometer-sized KBOs have instead a uniform ecliptic latitude distribution for -20 Degree-Sign < b < 20 Degree-Sign then N(r > 250 m) = 4.4{sup +5.8}{sub -2.8} Multiplication-Sign 10{sup 6} deg{sup -2}. This is the best measurement of the surface density of sub-kilometer-sized KBOs to date. (3) Assuming the KBO size distribution can be well described by a single power law given by N(> r){proportional_to}r{sup 1-q}, where N(> r) is the number of KBOs with radii greater than r, and q is the power-law index, we find q = 3.8 {+-} 0.2 and q = 3.6 {+-} 0.2 for a KBO ecliptic latitude distribution that follows the observed distribution for larger, 100-km-sized KBOs and a uniform KBO ecliptic latitude distribution for -20 Degree-Sign < b < 20 Degree-Sign , respectively. (4) Regardless of the exact power law, our results suggest that small KBOs are numerous enough to satisfy the required supply rate for the Jupiter family comets. (5) We can rule out a single power law below the break with q > 4.0 at 2{sigma}, confirming a strong deficit of sub-kilometer-sized KBOs compared to a population extrapolated from objects with r > 45 km. This suggests that small KBOs are undergoing collisional erosion and that the Kuiper Belt is a true analog to the dust producing debris disks observed around other stars.

  4. Will new horizons see dust clumps in the Edgeworth-Kuiper Belt?

    SciTech Connect (OSTI)

    Vitense, Christian; Krivov, Alexander V.; Löhne, Torsten

    2014-06-01

    Debris disks are thought to be sculptured by neighboring planets. The same is true for the Edgeworth-Kuiper debris disk, yet no direct observational evidence for signatures of giant planets in the Kuiper Belt dust distribution has been found so far. Here we model the dust distribution in the outer solar system to reproduce the dust impact rates onto the dust detector on board the New Horizons spacecraft measured so far and to predict the rates during the Neptune orbit traverse. To this end, we take a realistic distribution of trans-Neptunian objects to launch a sufficient number of dust grains of different sizes and follow their orbits by including radiation pressure, Poynting-Robertson and stellar wind drag, as well as the perturbations of four giant planets. In a subsequent statistical analysis, we calculate number densities and lifetimes of the dust grains in order to simulate a collisional cascade. In contrast to the previous work, our model not only considers collisional elimination of particles but also includes production of finer debris. We find that particles captured in the 3:2 resonance with Neptune build clumps that are not removed by collisions, because the depleting effect of collisions is counteracted by production of smaller fragments. Our model successfully reproduces the dust impact rates measured by New Horizons out to ?23 AU and predicts an increase of the impact rate of about a factor of two or three around the Neptune orbit crossing. This result is robust with respect to the variation of the vaguely known number of dust-producing scattered disk objects, collisional outcomes, and the dust properties.

  5. Hubble space telescope investigation of main-belt comet 133P/Elst-Pizarro

    SciTech Connect (OSTI)

    Jewitt, David; Ishiguro, Masateru; Weaver, Harold; Agarwal, Jessica; Mutchler, Max; Larson, Steven

    2014-05-01

    We report new observations of the prototype main-belt comet (active asteroid) 133P/Elst-Pizarro taken at high angular resolution using the Hubble Space Telescope. The object has three main components: (1) a point-like nucleus; (2) a long, narrow antisolar dust tail; and (3) a short, sunward anti-tail. There is no resolved coma. The nucleus has a mean absolute magnitude H{sub V} = 15.70 ± 0.10 and a light curve range ?V = 0.42 mag, the latter corresponding to projected dimensions 3.6 × 5.4 km (axis ratio 1.5:1) at the previously measured geometric albedo of 0.05 ± 0.02. We explored a range of continuous and impulsive emission models to simultaneously fit the measured surface brightness profile, width, and position angle of the antisolar tail. Preferred fits invoke protracted emission, over a period of 150 days or less, of dust grains following a differential power-law size distribution with index 3.25 ?q ? 3.5 and with a wide range of sizes. Ultra-low surface brightness dust projected in the sunward direction is a remnant from emission activity occurring in previous orbits, and consists of the largest (?cm-sized) particles. Ejection velocities of one-micron-sized particles are comparable to the ?1.8 m s{sup –1} gravitational escape speed of the nucleus, while larger particles are released at speeds less than the gravitational escape velocity. The observations are consistent with, but do not prove, a hybrid hypothesis in which mass loss is driven by gas drag from the sublimation of near-surface water ice, but escape is aided by centripetal acceleration from the rotation of the elongated nucleus. No plausible alternative hypothesis has been identified.

  6. Crustal structure of mountain belts and basins: Industry and academic collaboration at Cornell

    SciTech Connect (OSTI)

    Allmendinger, R.; Barazangi, M.; Brown, L. [Cornell Univ., Ithaca, NY (United States)] [and others

    1995-08-01

    Interdisciplinary investigations of the large-scale structure and evolution of key basins and orogenic belts around the world are the focal point of academic-industry interaction at Cornell. Ongoing and new initiatives with significant industry involvement include: Project INDEPTH (Interdisciplinary Deep Profiling of Tibet and the Himalayas), a multinational effort to delineate deep structure across the type example of active continent-continent collision. 300 km of deep reflection profiling was collected across the Himalaya: and southern Tibet Plateau in 1992 and 1994. CAP (Cornell Andes Project), a long-standing interdisciplinary effort to understand the structure and evolution of the Andes, with a focus on Argentina, Chile and Bolivia. A deep reflection profile is tentatively planned for 1997. Intra-plate Orogeny in the Middle East and North Africa is the focus of multidisciplinary regional syntheses of existing seismic reflection and other databases in Syria (Palmyrides)and Morocco (Atlas), with an emphasis on reactivation and inversion tectonics. Project URSEIS (Urals Reflection Seismic Experiment and Integrated Studies) is a collaboration with EUROPROBE to collect 500 km of vibroseis and dynamite deep reflection profiling across the southern Urals in 1995. Project CRATON, an element in COCORP`s systematic exploration of the continental US, is a nascent multi-disciplinary effort to understand the buried craton of the central US and the basins built upon it. Global Basins Research Network (GBRN) is a diversified observational and computational effort to image and model the movement of pore fluids in detail and on a regional scale for a producing oil structure in the Gulf of Mexico.

  7. Porous-electrode preparation method

    DOE Patents [OSTI]

    Arons, R.M.; Dusek, J.T.

    1981-09-17

    A porous sintered plaque is provided with a bimodal porosity that is especially well suited for use as an electrode within a molten carbonate fuel cell. The coarse porosity is sufficient for admitting gases into contact with the reaction surfaces while the fine porosity is wetted with and retains molten electrolyte on the reaction sites. The electrode structure is prepared by providing a very fine powder such as nickel oxide and blending the powder with a suitable decomposable binder to form a solid mass. The mass is comminuted into agglomerate size particles substantially larger than the fine oxide particles and formed into a cohesive compact for subsequent sintering. Sintering is carried out at sufficient conditions to bind the agglomerates together into a porous structure having both coarse and fine porosity. Where lithiated nickel oxide cathodes are prepared, the sintering conditions can be moderate enough to retain substantial quantities of lithium within the electrode for adequate conductivity.

  8. Preparation of superconductor precursor powders

    DOE Patents [OSTI]

    Bhattacharya, Raghunath (Littleton, CO)

    1998-01-01

    A process for the preparation of a precursor metallic powder composition for use in the subsequent formation of a superconductor. The process comprises the steps of providing an electrodeposition bath comprising an electrolyte medium and a cathode substrate electrode, and providing to the bath one or more soluble salts of one or more respective metals which are capable of exhibiting superconductor properties upon subsequent appropriate treatment. The bath is continually energized to cause the metallic and/or reduced particles formed at the electrode to drop as a powder from the electrode into the bath, and this powder, which is a precursor powder for superconductor production, is recovered from the bath for subsequent treatment. The process permits direct inclusion of all metals in the preparation of the precursor powder, and yields an amorphous product mixed on an atomic scale to thereby impart inherent high reactivity. Superconductors which can be formed from the precursor powder include pellet and powder-in-tube products.

  9. Preparation of energy storage materials

    DOE Patents [OSTI]

    Li, Lin Song (Los Alamos, NM); Jia, Quanxi (Los Alamos, NM)

    2003-01-01

    A process is provided for the preparation of a metallic oxide composite including mixing an aqueous solution of a water-soluble metal compound and colloidal silica, depositing the mixture upon a substrate, heating the mixture-coated substrates at temperatures from about 150.degree. C. to about 300.degree. C. for time sufficient to form a metallic oxide film, and, removing the silica from the metallic oxide film whereby a porous metal oxide structure is formed.

  10. Preparation Of Energy Storage Materials

    DOE Patents [OSTI]

    Li, Lin Song (Los Alamos, NM); Jia, Quanxi (Los Alamos, NM)

    2003-12-02

    A process is provided for the preparation of a metallic oxide composite including mixing an aqueous solution of a water-soluble metal compound and colloidal silica, depositing the mixture upon a substrate, heating the mixture-coated substrates at temperatures from about 150.degree. C. to about 300.degree. C. for time sufficient to form a metallic oxide film, and, removing the silica from the metallic oxide film whereby a porous metal oxide structure is formed.

  11. Method for preparing ceramic composite

    DOE Patents [OSTI]

    Alexander, Kathleen B. (Oak Ridge, TN); Tiegs, Terry N. (Lenoir City, TN); Becher, Paul F. (Oak Ridge, TN); Waters, Shirley B. (Knoxville, TN)

    1996-01-01

    A process for preparing ceramic composite comprising blending TiC particulates, Al.sub.2 O.sub.3 particulates and nickle aluminide and consolidating the mixture at a temperature and pressure sufficient to produce a densified ceramic composite having fracture toughness equal to or greater than 7 MPa m.sup.1/2, a hardness equal to or greater than 18 GPa.

  12. Method for preparing ceramic composite

    DOE Patents [OSTI]

    Alexander, K.B.; Tiegs, T.N.; Becher, P.F.; Waters, S.B.

    1996-01-09

    A process is disclosed for preparing ceramic composite comprising blending TiC particulates, Al{sub 2}O{sub 3} particulates and nickel aluminide and consolidating the mixture at a temperature and pressure sufficient to produce a densified ceramic composite having fracture toughness equal to or greater than 7 MPa m{sup 1/2}, a hardness equal to or greater than 18 GPa. 5 figs.

  13. Method of surface preparation of niobium

    DOE Patents [OSTI]

    Srinivasan-Rao, Triveni (Shoreham, NY); Schill, John F. (Ridge, NY)

    2003-01-01

    The present invention is for a method of preparing a surface of niobium. The preparation method includes polishing, cleaning, baking and irradiating the niobium surface whereby the resulting niobium surface has a high quantum efficiency.

  14. Preparation for Warmer Temperatures | Department of Energy

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

    Preparation for Warmer Temperatures Preparation for Warmer Temperatures April 2, 2014 - 11:05am Addthis Ceiling fans are a great way to efficiently cool your house in the summer. |...

  15. Stormwater Pollution Prevention Plan Prepared by

    E-Print Network [OSTI]

    Eisen, Michael

    Stormwater Pollution Prevention Plan Prepared by: Environment, Health, Safety, and Security .....................................................16 3.0 Potential Sources of Pollution

  16. Preparing for the Arrival of Electric Vehicle

    Broader source: Energy.gov [DOE]

    This webinar covers how to prepare for electric vehicles and elements of developing an EV infrastructure plan.

  17. The formation of the solar system by gravitational instability: Prediction of a new planet or another Kuiper-type belt

    E-Print Network [OSTI]

    Evgeny Griv; Michael Gedalin

    2004-03-16

    The early gas-dust solar nebula is considered: the gasdynamic theory is used to study the gravitational Jeans-type instability in its protoplanetary disk. The implications for the origin of the solar system are discussed. It is shown that a collective process, forming the basis of the gravitational instability hypothesis, solves with surprising simplicity the two main problems of the dynamical characteristics of the system, which are associated with its observed spacing and orbital momentum distribution. The analysis is found to imply the existence of a new planet (or another Kuiper-type belt) at a mean distance from the Sun of 87 AU.

  18. Air Dispersion Modeling of Mine Waste in the Southeast Missouri Old Lead Belt

    SciTech Connect (OSTI)

    Abbott, Michael Lehman

    1999-10-01

    Past lead ore processing conducted in the Southeast Missouri Old Lead Belt since the 1700s has left numerous large areas of lead contamination in elevated piles of fine gravel waste called “chat” and dried-out tailings ponds. Wind suspension and atmospheric dispersion are known to transport these materials to the surrounding communities where the lead could pose a human health threat through inhalation or ingestion of the deposited contamination. The purpose of this study was to estimate potential wind suspension rates, perform dispersion modeling of the tailings and chat sources, and determine ground surface deposition rates and potential soil concentrations of lead in the surrounding areas. The results can be used to prioritize soil sampling locations, site air monitors, help identify the source of soil lead contamination, and to help develop remediation plans. Numerous, large complex sources in the region were parameterized into 33 area sources with the aid of digital aerial photos, digitized typographic maps, Geographic Information Systems (GIS) software, and site inspections. An AP-42 particulate emission model was used to estimate lower- and upper-bound hourly emission rates using six years of hourly wind speed data obtained from the St. Louis Airport. The emissions model accounted for wind speed, precipitation, source-specific aggregate size, fraction of vegetation cover, and site-specific lead concentrations. An alternative simplified method to calculate emissions from elevated chat piles was developed. The Fugitive Dust Model (FDM) was then used to calculate long-term average and maximum 24-hour deposition rates of lead over a 200 km2 region. Soil concentrations were estimated from modeled deposition rates, time of deposition (80 y) and an assumed surface (0-5.08 cm) mixing depth. Model performance was evaluated by comparing lower- and upper- bound modeled predictions to both air and soil sampling data obtained at two sites. The predicted-to-observed (P/O) ratios calculated using the geometric mean of the lower- and upper-bound modeled concentrations ranged from a low of 0.84 at 300 m to a high of 1.4 at 1800 m, with an average of 1.1. The P/O ratios tended to increase slightly at distances beyond about 1 km. These P/O ratios demonstrate exceptional model performance for the particular sampling transect (location and direction) investigated.

  19. Electron loss rates from the outer radiation belt caused by the filling of the outer plasmasphere: the calm before the storm

    SciTech Connect (OSTI)

    Borovsky, Joseph E [Los Alamos National Laboratory; Denton, Michael H [LANCASTER UNIV

    2009-01-01

    Measurements from 7 spacecraft in geosynchronous orbit are analyzed to determine the decay rate of the number density of the outer electron radiation belt prior to the onset of high-speed-stream-driven geomagnetic storms. Superposed-data analysis is used wan(?) a collection of 124 storms. When there is a calm before the storm, the electron number density decays exponentially before the storm with a 3.4-day e-folding time: beginning about 4 days before storm onset, the density decreases from {approx}4x10{sup -4} cm{sup -3} to {approx}1X 10{sup -4} cm{sup -3}. When there is not a calm before the storm, the number-density decay is very smalL The decay in the number density of radiation-belt electrons is believed to be caused by pitch-angle scattering of electrons into the atmospheric loss cone as the outer plasmasphere fills during the calms. While the radiation-belt electron density decreases, the temperature of the electron radiation belt holds approximately constant, indicating that the electron precipitation occurs equally at all energies. Along with the number density decay, the pressure of the outer electron radiation belt decays and the specific entropy increases. From the measured decay rates, the electron flux to the atmosphere is calculated and that flux is 3 orders of magnitude less than thermal fluxes in the magnetosphere, indicating that the radiation-belt pitch-angle scattering is 3 orders weaker than strong diffusion. Energy fluxes into the atmosphere are calculated and found to be insufficient to produce visible airglow.

  20. PSW1-C0.2-D0.1-E2.4-F0.1-PSRB2-0021-02 SOLAR WIND-DRIVEN ELECTRON RADIATION BELT

    E-Print Network [OSTI]

    PSW1-C0.2-D0.1-E2.4-F0.1-PSRB2-0021-02 SOLAR WIND-DRIVEN ELECTRON RADIATION BELT RESPONSE FUNCTIONS linear filters, to remove unwanted "col- ored noise" from solar wind and radiation belt electron data prediction filters to represent the driven portion of the linear dynamics that describe the coupling between