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1

Cosmic Frontier | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Cosmic Frontier High Energy Physics (HEP) HEP Home About Research Snowmass P5 Planning Process Energy Frontier Intensity Frontier Cosmic Frontier Cosmic Frontier: More...

2

Accelerators for Intensity Frontier Research  

SciTech Connect

In 2008, the Particle Physics Project Prioritization Panel identified three frontiers for research in high energy physics, the Energy Frontier, the Intensity Frontier, and the Cosmic Frontier. In this paper, I will describe how Fermilab is configuring and upgrading the accelerator complex, prior to the development of Project X, in support of the Intensity Frontier.

Derwent, Paul; /Fermilab

2012-05-11T23:59:59.000Z

3

Intensity Frontier Instrumentation  

E-Print Network (OSTI)

This report summarizes findings of the 2013 Snowmass Community Summer Study Instrumentation Frontier's subgroup on the Intensity Frontier. This report is directed at identifying instrumentation R&D needed to support particle physics research over the coming decades at the Intensity Frontier.

S. H. Kettell; R. A. Rameika; R. S. Tschirhart

2013-09-26T23:59:59.000Z

4

Frontiers in Cosmic Rays  

E-Print Network (OSTI)

This rapporteur review covers selected results presented in the Parallel Session HEA2 (High Energy Astrophysics 2) of the 10th Marcel Grossmann Meeting on General Relativity, held in Rio de Janeiro, Brazil, July 2003. The subtopics are: ultra high energy cosmic ray anisotropies, the possible connection of these energetic particles with powerful gamma ray bursts, and new exciting scenarios with a strong neutrino-nucleon interaction in the atmosphere.

Luis A. Anchordoqui; Charles D. Dermer; Andreas Ringwald

2004-02-27T23:59:59.000Z

5

Fermilab | Science at Fermilab | Experiments & Projects | Cosmic Frontier |  

NLE Websites -- All DOE Office Websites (Extended Search)

Intensity Frontier Intensity Frontier Cosmic Frontier Experiments at the Cosmic Frontier How it works Questions for the Universe Scientific results Experiments CDMS COUPP GammeV Pierre Auger SDSS Dark Energy Survey Proposed Projects and Experiments Cosmic Frontier CDMS CDMS Researchers on the Cryogenic Dark Matter Search, or CDMS, experiment are searching for WIMPs, which may make up dark matter. Researchers built the CDMS detector to identify WIMPs through their interactions with nuclei in a section of the detector made of germanium crystals. When a nucleus is hit, it recoils, causing the whole germanium crystal to vibrate. Theorists expect WIMPs to interact only once a year in each kilogram of space, and the energy caused by the nuclear recoil is very low. So the CDMS detector must distinguish between the effects of WIMP interactions and

6

Intensity Frontier Instrumentation  

SciTech Connect

The fundamental origin of flavor in the Standard Model (SM) remains a mystery. Despite the roughly eighty years since Rabi asked “Who ordered that?” upon learning of the discovery of the muon, we have not understood the reason that there are three generations or, more recently, why the quark and neutrino mixing matrices and masses are so different. The solution to the flavor problem would give profound insights into physics beyond the Standard Model (BSM) and tell us about the couplings and the mass scale at which the next level of insight can be found. The SM fails to explain all observed phenomena: new interactions and yet unseen particles must exist. They may manifest themselves by causing SM reactions to differ from often very precise predictions. The Intensity Frontier (1) explores these fundamental questions by searching for new physics in extremely rare processes or those forbidden in the SM. This often requires massive and/or extremely finely tuned detectors.

Kettell S.; Rameika, R.; Tshirhart, B.

2013-09-24T23:59:59.000Z

7

Experiments at the Cosmic Frontier | U.S. DOE Office of Science (SC)  

NLE Websites -- All DOE Office Websites (Extended Search)

Cosmic Frontier Cosmic Frontier High Energy Physics (HEP) HEP Home About Research Facilities Facility Ops Experiments at the Energy Frontier Experiments at the Intensity Frontier Experiments at the Cosmic Frontier Projects, Missions, and Status HEP User Facilities Science Highlights Benefits of HEP Funding Opportunities Advisory Committees News & Resources Contact Information High Energy Physics U.S. Department of Energy SC-25/Germantown Building 1000 Independence Ave., SW Washington, DC 20585 P: (301) 903-3624 F: (301) 903-2597 E: sc.hep@science.doe.gov More Information » Facilities Experiments at the Cosmic Frontier Print Text Size: A A A RSS Feeds FeedbackShare Page The Cosmic Frontier reveals the nature of dark matter and dark energy by using particles from space to explore new phenomena. Cosmic rays in the

8

Frontiers  

NLE Websites -- All DOE Office Websites (Extended Search)

Frontiers Frontiers of Discovery Fermi National Accelerator Laboratory T A B L E O F C O N T E N T S 06 Energy Frontier 08 CDF 09 DZero 10 CMS 11 LHC Remote Operations 12 SRF Technology 12 ILC 13 Muon Collider 14 Intensity Frontier 16 NOνA 17 MINOS 18 MicroBooNE 18 MiniBooNE 19 MINERνA 20 SRF Test Accelerator 21 Project X 22 LBNE 22 Liquid Argon 23 Mu2e 24 Cosmic Frontier 26 Pierre Auger 27 Dark Energy Survey 28 DAMIC 29 CDMS 30 COUPP 31 Holometer Robert Wilson, Fermilab's founding director, introduced the first American bison, a bull and four cows, to the Fermilab site in 1969. The bison symbolize the laboratory's historic connection to the great Midwestern prairie and Fermilab's role at the frontiers of research in particle physics. Frontiers of discovery What is the nature of the universe? What are matter and

9

Energy Frontier | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Energy Frontier High Energy Physics (HEP) HEP Home About Research Snowmass P5 Planning Process Energy Frontier Intensity Frontier Cosmic Frontier Theoretical Physics Advanced...

10

Intensity Frontier: More Information | U.S. DOE Office of Science (SC)  

NLE Websites -- All DOE Office Websites (Extended Search)

Intensity Intensity Frontier » Intensity Frontier: More Information High Energy Physics (HEP) HEP Home About Research Snowmass / P5 Planning Process Intensity Frontier Cosmic Frontier Theoretical Physics Advanced Technology R&D Accelerator R&D Stewardship Research Highlights .pdf file (13.1MB) Questions for the Universe Accomplishments Facilities Science Highlights Benefits of HEP Funding Opportunities Advisory Committees News & Resources Contact Information High Energy Physics U.S. Department of Energy SC-25/Germantown Building 1000 Independence Ave., SW Washington, DC 20585 P: (301) 903-3624 F: (301) 903-2597 E: sc.hep@science.doe.gov More Information » Intensity Frontier Intensity Frontier: More Information Print Text Size: A A A RSS Feeds FeedbackShare Page Experiments at the Intensity Frontier aim to transform our understanding of

11

Experiments at the Intensity Frontier | U.S. DOE Office of Science (SC)  

NLE Websites -- All DOE Office Websites (Extended Search)

Intensity Frontier Intensity Frontier High Energy Physics (HEP) HEP Home About Research Facilities Facility Ops Experiments at the Energy Frontier Experiments at the Intensity Frontier Experiments at the Cosmic Frontier Projects, Missions, and Status HEP User Facilities Science Highlights Benefits of HEP Funding Opportunities Advisory Committees News & Resources Contact Information High Energy Physics U.S. Department of Energy SC-25/Germantown Building 1000 Independence Ave., SW Washington, DC 20585 P: (301) 903-3624 F: (301) 903-2597 E: sc.hep@science.doe.gov More Information » Facilities Experiments at the Intensity Frontier Print Text Size: A A A RSS Feeds FeedbackShare Page The Intensity Frontier, accessed with a combination of intense particle beams and highly sensitive detectors, offers a second, unique investigation

12

Fermilab | Science at Fermilab | Frontiers of Particle Physics  

NLE Websites -- All DOE Office Websites (Extended Search)

Diaries Frontiers of Particle Physics Frontiers of Particle Physics Three frontiers: energy, intensity and cosmic At Fermilab, a robust scientific program pushes forward on...

13

Fermilab | Science at Fermilab | Experiments & Projects | Cosmic Frontier  

NLE Websites -- All DOE Office Websites (Extended Search)

photo-cosmic photo-cosmic Cosmic Frontier Particle physics experiments at the Cosmic Frontier use the cosmos as a laboratory to investigate the fundamental laws of physics. Researchers use detectors to study particles from space as they approach and enter our atmosphere in forms such as cosmic rays, gamma rays and neutrinos emitted by the sun. These experiments allow researchers to test theories about how the universe was formed, what it is made of and what its future holds. Experiments at the Cosmic Frontier may have the best chance of discovering the nature of dark matter and dark energy. Theorists have concluded that these two mysterious materials constitute 96 percent of the universe and may be responsible for its formation and accelerating expansion. WIMPS and dark matter

14

Fermilab | Science at Fermilab | Experiments & Projects | Intensity...  

NLE Websites -- All DOE Office Websites (Extended Search)

to main content Science at Fermilab Frontiers of Particle Physics Experiments & Projects Energy Frontier Tevatron at Fermilab Fermilab and the LHC Intensity Frontier Cosmic...

15

Intensity Frontier | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

more detail may lead to the answers to a number of big questions in particle physics. Quantum mechanics is what allows Intensity Frontier research to answer these questions by...

16

For Physicists | Fellowships & Awards | Intensity Frontier Fellows  

NLE Websites -- All DOE Office Websites (Extended Search)

Application Info Application Info Applications must include a curriculum vitae, and a selected publication list. In addition we request a two-page proposal describing the major contribution that will be made to the Intensity Frontier during the Fellowship, current compensation, and requested dates of support. Applicants holding postdoctoral positions should supply two letters of reference. Applications for awards beginning in 2014 will be accepted until 22 November, 2013. It is anticipated that a second round of applications will be solicited in spring 2014. Applicants should be notified by 20 December 2013. Applications should be made via: Online Application Further queries should be sent to: send email Related Links Fermilab Intensity Frontier Department NOvA Experiment

17

Fundamental physics at the intensity frontier. Report of the workshop held December 2011 in Rockville, MD.  

SciTech Connect

Particle physics aims to understand the universe around us. The Standard Model of particle physics describes the basic structure of matter and forces, to the extent we have been able to probe thus far. However, it leaves some big questions unanswered. Some are within the Standard Model itself, such as why there are so many fundamental particles and why they have different masses. In other cases, the Standard Model simply fails to explain some phenomena, such as the observed matter-antimatter asymmetry in the universe, the existence of dark matter and dark energy, and the mechanism that reconciles gravity with quantum mechanics. These gaps lead us to conclude that the universe must contain new and unexplored elements of Nature. Most of particle and nuclear physics is directed towards discovering and understanding these new laws of physics. These questions are best pursued with a variety of approaches, rather than with a single experiment or technique. Particle physics uses three basic approaches, often characterized as exploration along the cosmic, energy, and intensity frontiers. Each employs different tools and techniques, but they ultimately address the same fundamental questions. This allows a multi-pronged approach where attacking basic questions from different angles furthers knowledge and provides deeper answers, so that the whole is more than a sum of the parts. A coherent picture or underlying theoretical model can more easily emerge, to be proven correct or not. The intensity frontier explores fundamental physics with intense sources and ultra-sensitive, sometimes massive detectors. It encompasses searches for extremely rare processes and for tiny deviations from Standard Model expectations. Intensity frontier experiments use precision measurements to probe quantum effects. They typically investigate very large energy scales, even higher than the kinematic reach of high energy particle accelerators. The science addresses basic questions, such as: Are there new sources of CP violation? Is there CP violation in the leptonic sector? Are neutrinos their own antiparticles? Do the forces unify? Is there a weakly coupled hidden sector that is related to dark matter? Do new symmetries exist at very high energy scales? To identify the most compelling science opportunities in this area, the workshop Fundamental Physics at the Intensity Frontier was held in December 2011, sponsored by the Office of High Energy Physics in the US Department of Energy Office of Science. Participants investigated the most promising experiments to exploit these opportunities and described the knowledge that can be gained from such a program. The workshop generated much interest in the community, as witnessed by the large and energetic participation by a broad spectrum of scientists. This document chronicles the activities of the workshop, with contributions by more than 450 authors. The workshop organized the intensity frontier science program along six topics that formed the basis for working groups: experiments that probe (i) heavy quarks, (ii) charged leptons, (iii) neutrinos, (iv) proton decay, (v) light, weakly interacting particles, and (vi) nucleons, nuclei, and atoms. The conveners for each working group included an experimenter and a theorist working in the field and an observer from the community at large. The working groups began their efforts well in advance of the workshop, holding regular meetings and soliciting written contributions. Specific avenues of exploration were identified by each working group. Experiments that study rare strange, charm, and bottom meson decays provide a broad program of measurements that are sensitive to new interactions. Charged leptons, particularly muons and taus, provide a precise probe for new physics because the Standard Model predictions for their properties are very accurate. Research at the intensity frontier can reveal CP violation in the lepton sector, and elucidate whether neutrinos are their own antiparticles. A very weakly coupled hidden-sector that may comprise the dark matter in the univ

Hewett, J.L.; Weerts, H.; Brock, R.; Butler, J.N.; Casey, B.C.K.; Lu, Z.T.; Wagner, C.E.M.; Dietrich, M.R.; Djurcic, Z.; Goodman, M.; Green, J.P.; Holt, R.J.; Mueller, P.; Paley, J.; Reimer, P.; Singh, J.; Upadhye, A. (High Energy Physics); ( PHY); (Stanford Linear Accelerator Center); (Univ. of Michigan); (Fermi National Accelerator Laboratory)

2012-06-05T23:59:59.000Z

18

Charting the New Frontier of the Cosmic Microwave Background Polarization  

E-Print Network (OSTI)

The anisotropies of the cosmic microwave background are a gold mine for cosmology and fundamental physics. ESA's Planck satellite should soon extract all information from the temperature vein but will be limited concerning the measurement of the degree of polarization of the anisotropies. This polarization information allows new independent tests of the standard cosmological paradigm, improves knowledge of cosmological parameters and last but not least is the best window available for constraining the physics of the very early universe, particularly the expected background of primordial gravitational waves. But exploiting this vein will be a challenge, since the sensitivity required is {\\em at least} 10 times better than what Planck might achieve at best, with the necessary matching level of control of all systematics effects, both instrumental and astrophysical (foregrounds). We here recall the cosmological context and the case for CMB polarization studies. We also briefly introduce the SAMPAN project, a des...

Bouchet, F R; Camus, P; Désert, F X; Piat, M; Ponthieu, N; Camus, Ph.

2005-01-01T23:59:59.000Z

19

Fermilab | Science at Fermilab | Experiments & Projects | Cosmic Frontier |  

NLE Websites -- All DOE Office Websites (Extended Search)

Pierre Auger Pierre Auger Pierre Auger Observatory at night Pierre Auger Observatory at night On the pampas of western Argentina, the Pierre Auger cosmic-ray observatory studies the effects of collisions of high-energy particles with Earth's atmosphere over an area of 3,000 square kilometers. When fast-moving particles strike air molecules in the Earth's atmosphere, debris flies from the collision in what is called an air shower. Fragments hit other air molecules in a cascade that continues until the energy of the original particle is spread among millions or even billions of particles raining down on Earth. By studying these air showers, physicists can investigate the source of the original particles. The rate at which particles with energies above 1019 electron volts fall

20

Low Background Materials and Assay - A Supplement to the Cosmic Frontier CF1 Summary  

E-Print Network (OSTI)

This White Paper provides a supplement to the Snowmass Summary from CF1 (Cosmic Frontier WIMP Direct Detection). It was largely prepared during the August 2013 Community Planning Meeting and relies on information gathered from the larger dark matter community. It is a more detailed answer to the CF1 Charge: "Identify the common infrastructure required to meet the scientific and technical goals of dark matter direct detection." The community as a whole recognizes that sensitive searches for WIMPs require identification, quantification, and procurement of radiopure materials. The lack of sufficient resources in this area is a major project risk for future experiments and can limit scientific reach

J. Cooley; P. Cushman; E. W. Hoppe; J. L. Orrell; R. W. Schnee

2013-11-13T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


21

Issues and R&D Required for the Intensity Frontier Accelerators  

E-Print Network (OSTI)

We discuss main issues and R&D Required for the Intensity Frontier Accelerators and therefore provide input for the 2013 APS/DPF Community Summer Study (Snowmass-2013).

V. Shiltsev; S. Henderson; P. Hurh; I. Kourbanis; V. Lebedev

2013-05-29T23:59:59.000Z

22

Report of the Snowmass 2013 Computing Frontier working group on Lattice Field Theory -- Lattice field theory for the energy and intensity frontiers: Scientific goals and computing needs  

E-Print Network (OSTI)

This is the report of the Computing Frontier working group on Lattice Field Theory prepared for the proceedings of the 2013 Community Summer Study ("Snowmass"). We present the future computing needs and plans of the U.S. lattice gauge theory community and argue that continued support of the U.S. (and worldwide) lattice-QCD effort is essential to fully capitalize on the enormous investment in the high-energy physics experimental program. We first summarize the dramatic progress of numerical lattice-QCD simulations in the past decade, with some emphasis on calculations carried out under the auspices of the U.S. Lattice-QCD Collaboration, and describe a broad program of lattice-QCD calculations that will be relevant for future experiments at the intensity and energy frontiers. We then present details of the computational hardware and software resources needed to undertake these calculations.

Blum, T; Holmgren, D; Brower, R; Catterall, S; Christ, N; Kronfeld, A; Kuti, J; Mackenzie, P; Neil, E T; Sharpe, S R; Sugar, R

2013-01-01T23:59:59.000Z

23

Report of the Snowmass 2013 Computing Frontier working group on Lattice Field Theory -- Lattice field theory for the energy and intensity frontiers: Scientific goals and computing needs  

E-Print Network (OSTI)

This is the report of the Computing Frontier working group on Lattice Field Theory prepared for the proceedings of the 2013 Community Summer Study ("Snowmass"). We present the future computing needs and plans of the U.S. lattice gauge theory community and argue that continued support of the U.S. (and worldwide) lattice-QCD effort is essential to fully capitalize on the enormous investment in the high-energy physics experimental program. We first summarize the dramatic progress of numerical lattice-QCD simulations in the past decade, with some emphasis on calculations carried out under the auspices of the U.S. Lattice-QCD Collaboration, and describe a broad program of lattice-QCD calculations that will be relevant for future experiments at the intensity and energy frontiers. We then present details of the computational hardware and software resources needed to undertake these calculations.

T. Blum; R. S. Van de Water; D. Holmgren; R. Brower; S. Catterall; N. Christ; A. Kronfeld; J. Kuti; P. Mackenzie; E. T. Neil; S. R. Sharpe; R. Sugar

2013-10-23T23:59:59.000Z

24

Experiments at the Energy Frontier | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Energy Frontier Energy Frontier High Energy Physics (HEP) HEP Home About Research Facilities Facility Ops Experiments at the Energy Frontier Experiments at the Intensity Frontier Experiments at the Cosmic Frontier Projects, Missions, and Status HEP User Facilities Science Highlights Benefits of HEP Funding Opportunities Advisory Committees News & Resources Contact Information High Energy Physics U.S. Department of Energy SC-25/Germantown Building 1000 Independence Ave., SW Washington, DC 20585 P: (301) 903-3624 F: (301) 903-2597 E: sc.hep@science.doe.gov More Information » Facilities Experiments at the Energy Frontier Print Text Size: A A A RSS Feeds FeedbackShare Page The Energy Frontier directly explores the fundamental constituents and architecture of the universe. Here accelerators produce the highest-energy

25

THE COSMIC-RAY INTENSITY NEAR THE ARCHEAN EARTH  

Science Conference Proceedings (OSTI)

We employ three-dimensional state-of-the-art magnetohydrodynamic models of the early solar wind and heliosphere and a two-dimensional model for cosmic-ray transport to investigate the cosmic-ray spectrum and flux near the Archean Earth. We assess how sensitive the cosmic-ray spectrum is to changes in the sunspot placement and magnetic field strength, the large-scale dipole magnetic field strength, the wind ram pressure, and the Sun's rotation period. Overall, our results confirm earlier work that suggested the Archean Earth would have experienced a greatly reduced cosmic-ray flux than is the case today. The cosmic-ray reduction for the early Sun is mainly due to the shorter solar rotation period and tighter winding of the Parker spiral, and to the different surface distribution of the more active solar magnetic field. These effects lead to a global reduction of the cosmic-ray flux at 1 AU by up to two orders of magnitude or more. Variations in the sunspot magnetic field have more effect on the flux than variations in the dipole field component. The wind ram pressure affects the cosmic-ray flux through its influence on the size of the heliosphere via the pressure balance with the ambient interstellar medium. Variations in the interstellar medium pressure experienced by the solar system in orbit through the Galaxy could lead to order of magnitude changes in the cosmic-ray flux at Earth on timescales of a few million years.

Cohen, O.; Drake, J. J. [Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 (United States); Kota, J. [Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721-0092 (United States)

2012-11-20T23:59:59.000Z

26

The Impact of Intrinsic Heavy Quark Distributions in the Proton on New Physics Searches at the High Intensity Frontier  

SciTech Connect

The possibility of an intense proton facility, at 'Project X' or elsewhere, will provide many new opportunities for searches for physics beyond the Standard Model. A Project X can serve a yet broader role in the search for new physics, and in this note we highlight the manner in which thus-enabled studies of the flavor structure of the proton, particularly of its intrinsic heavy quark content, facilitate other direct and indirect searches for new physics. Intrinsic heavy quarks in both light and heavy hadrons play a key role in searches for physics BSM with hadrons - and their study at the Intensity Frontier may prove crucial to establishing its existence.

Brodsky, Stanley; /SLAC; Gardner, Susan; /Kentucky U.

2012-02-16T23:59:59.000Z

27

Probing TeV Left-Right Seesaw at Energy and Intensity Frontiers: a Snowmass White Paper  

E-Print Network (OSTI)

We discuss ways to probe the origin of neutrino masses at the Energy and Intensity frontiers, in TeV-scale left-right seesaw models where small neutrino masses arise via type-I seesaw mechanism. We consider generic ('vanilla') version of such models as well as a version which leads to 'large' light-heavy neutrino mixing while keeping the neutrino masses small in a natural manner. We point out specific observable implications of these classes of models at the LHC as well as in searches for lepton flavor violating processes such as $\\mu\\to e\\gamma$ and $\\mu\\to 3e$, and also in searches for lepton number violating neutrinoless double beta decay.

P. S. Bhupal Dev; R. N. Mohapatra

2013-08-09T23:59:59.000Z

28

Fermilab | Science at Fermilab | Experiments & Projects | Intensity  

NLE Websites -- All DOE Office Websites (Extended Search)

Intensity Frontier Intensity Frontier Experiments at the Intensity Frontier ArgoNeuT MINERvA MiniBooNE MINOS NOvA LBNE Cosmic Frontier Proposed Projects and Experiments ArgoNeuT ArgoNeut detector at Proton Assembly Building Intensity Frontier ArgoNeuT The Argon Neutrino Teststand or ArgoNeuT detector, nicknamed for Jason and the Argonauts of Greek mythology, is a liquid argon neutrino detector at Fermilab. Argon is a noble, non-toxic element that in its gaseous form constitutes about 1 percent of air. It exists as a colorless liquid only in the narrow temperature range of minus 186 to minus 189 degrees Celsius. Neutrinos passing through a large volume of argon can interact with an argon atom, producing secondary particles such as muons and protons, which then ionize other argon atoms. An electric field within the detector causes

29

Strong variations of cosmic ray intensity during thunderstorms and associated pulsations of the geomagnetic field  

E-Print Network (OSTI)

Strong variations of the intensity of secondary cosmic rays during thunderstorms are found to be accompanied in some cases by very clear pulsations of the geomagnetic field. The experiment is carried out in the Baksan Valley, North Caucasus, the Carpet air shower array being used as a particle detector. Magnetic field measurements are made with high-precision magnetometers located deep underground in the tunnel of the Baksan Neutrino Observatory, several kilometers apart from the air shower array.

Kanonidi, K Kh; Lidvansky, A S; Sobisevich, L E

2011-01-01T23:59:59.000Z

30

Fermilab | Science at Fermilab | Experiments & Projects | Energy Frontier |  

NLE Websites -- All DOE Office Websites (Extended Search)

Tevatron at Fermilab CDF DZero Fermilab involvement with the Large Hadron Collider Intensity Frontier Cosmic Frontier Works in Progress DZero detector in the Collision Hall DZero detector in the Collision Hall. A silicon strip disk for the DZero experiment's silicon tracker A silicon strip disk for the DZero experiment's silicon tracker. Energy Frontier DZero How it works DZero is one of two detectors positioned along the four-mile Tevatron accelerator ring.It takes its name from its location on the ring, D0. Physicists use the detector to study the array of particles and forces in nature by recording data about collisions of protons and anti-protons in the accelerator. The 5,500-ton detector sits more than four stories tall and is composed of more than 1 million individual detector elements.

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Fermilab | Science at Fermilab | Experiments & Projects | Energy Frontier |  

NLE Websites -- All DOE Office Websites (Extended Search)

CDF DZero Fermilab involvement with the Large Hadron Collider Intensity Frontier Cosmic Frontier Works in Progress CDF silicon vertex detector being installed in 2001 CDF silicon vertex detector being installed in 2001. Drawing of the CDF detector Drawing of the CDF detector. Energy Frontier CDF How it works CDF is one of two detectors positioned along the four-mile Tevatron accelerator ring. Physicists use the detector to study the array of particles and forces within the atom by recording data about collisions of protons and anti-protons in the machine. The 4,500-ton detector sits more than four stories tall and is composed of more than 1 million individual detector elements. Beams of protons and antiprotons collide at the center of CDF at nearly the speed of light, creating flashes of energy that condense into particles

32

Fermilab | Science at Fermilab | Experiments & Projects | Energy Frontier |  

NLE Websites -- All DOE Office Websites (Extended Search)

CDF DZero Fermilab involvement with the Large Hadron Collider Intensity Frontier Cosmic Frontier Works in Progress Energy Frontier Tevatron Before shutting down on Sept. 29, 2011, the Tevatron was the world's largest proton-antiproton collider. Residing at Fermilab, the Tevatron accelerated and stored beams of protons and antiprotons traveling in opposite directions around an underground ring four miles in circumference at almost the speed of light before colliding them at the center of two detectors. The detectors, called CDF, for Collider Detector at Fermilab, and DZero, named for its location on the accelerator ring, contain many detection subsystems that identified the different types of particles emerging from the collisions. Scientists explored the structure of matter, space and time

33

Fermilab | Science at Fermilab | Experiments & Projects | Energy Frontier  

NLE Websites -- All DOE Office Websites (Extended Search)

Tevatron at Fermilab Fermilab involvement with the Large Hadron Collider Intensity Frontier Cosmic Frontier Proposed Projects and Experiments Inside view of drift tube in older 200 MeV section of Linac. Inside view of drift tube in older 200 MeV section of Linac. Energy Frontier Collider Physics To explore the smallest particles, those inside an atom, physicists use the largest of scientific instruments, particle accelerators with a length measured in miles. These giant tools of particle physics can accelerate particles to very close to the speed of light. All particle accelerators start from the principle that electrically charged objects exert a force on each other--opposite charges attract; like charges repel. If there are no other forces keeping the objects in place,

34

Intensity-Frontier Antiproton Physics with The Antiproton Annihilation Spectrometer (TAPAS) at Fermilab  

SciTech Connect

The Fermilab Antiproton Source is the world's most intense source of antimatter. With the Tevatron program now behind us, this unique facility can help make the case for Fermilab's continued accelerator operations. The Antiproton Source can be used for unique, dedicated antimatter studies, including medium-energy {bar p}-annihilation experiments. We propose to assemble a powerful, yet cost-effective, solenoidal magnetic spectrometer for antiproton-annihilation events, and to use it at the Fermilab Antiproton Accumulator to measure the charm production cross section, study rare hyperon decays, search for hyperon CP asymmetry, precisely measure the properties of several charmonium and nearby states, and make the first measurements of the Drell-Yan continuum in medium-energy antiproton annihilation. Should the charm production cross section be as large as some have proposed, we will also be able to measure D{sup 0}-{bar D}{sup 0} mixing with high precision and discover (or sensitively limit) charm CP violation. The observation of charm or hyperon CP violation would be evidence for physics beyond the Standard Model, with possible implications for the origin of the baryon asymmetry of the universe - the question of what happened to all the antimatter that must have been produced in the Big Bang. The experiment will be carried out by an international collaboration and will require some four years of running time. As possibly the sole hadron experiment in progress at Fermilab during that time, it will play an important role in maintaining a broad particle physics program at Fermilab and in the U.S. It will thus help us to continue attracting creative and capable young people into science and technology, and introducing them to the important technologies of accelerators, detectors, and data acquisition and analysis - key roles in society that accelerator-based particle physics has historically played.

Apollinari, Giorgio; /Fermilab; Asner, David M.; /PNL, Richland; Baldini, Wander; /INFN, Ferrara; Bartoszek, Larry; Broemmelsiek, Daniel R.; Brown, Charles N.; /Fermilab; Chakravorty, Alak; /St. Xavier U., Chicago; Colas, Paul; /Saclay; Derwent, Paul; /Fermilab; Drutskoy, Alexey; /Moscow, ITEP; Fortner, Michael; /Northern Illinois U. /Saclay /Indian Inst. Tech., Hyderabad

2011-11-01T23:59:59.000Z

35

Cosmic  

NLE Websites -- All DOE Office Websites (Extended Search)

below about 10 GeV. In addition, the lower-energy cosmic rays are affected by the geomagnetic field, which they must penetrate to reach the top of the atmosphere. Thus the...

36

cosmicfrontiermoreinfo | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Cosmic Frontier: More Information High Energy Physics (HEP) HEP Home About Research Snowmass P5 Planning Process Energy Frontier Intensity Frontier Cosmic Frontier Cosmic...

37

Summary of the cosmic-ray intensity during the solar-terrestrial events of 16 February and 24-28 April 1984  

SciTech Connect

A brief summary is presented of the ground-level solar cosmic-ray event on 16 February 1984 and of the Forbush decrease in cosmic-ray intensity associate with the flare of 24 April and subsequent geomagnetic disturbance on 26-28 April 1984.

Shea, M.A.

1987-07-01T23:59:59.000Z

38

Sky-maps of the sidereal anisotropy of galactic cosmic ray intensity and its energy dependence  

E-Print Network (OSTI)

We analyze the sidereal daily variations observed between 1985 and 2006 at Matsushiro, Japan (MAT) and between 1993 and 2005 at Liapootah, Tasmania (LPT). These stations comprise the two hemisphere network (THN) of underground muon detectors in Japan and Australia. Yearly mean harmonic vectors at MAT and LPT are more or less stable without any significant change in phase and amplitude in correlation with either the solar activity- or magnetic-cycles. In this paper, therefore, we analyze the average anisotropy over the entire observation periods, i.e. 1985-2006 for MAT and 1993-2005 for LPT. We apply to the THN data a best-fitting analysis based on a model anisotropy in space identical to that adopted by Amenomori et al. (2007) for Tibet III data. The median energies of primary cosmic rays recorded are ~0.5 TeV for THN and ~5 TeV for the Tibet III experiment. It is shown that the intensity distribution of the best-fit anisotropy is quite similar to that derived from Tibet III data, regardless of the order of magnitude difference in energies of primary particles. This, together with the THN observations, confirms that the analysis by Amenomori et al. (2007) based on the Tibet III experiment in the northern hemisphere is not seriously biased. The best-fit amplitudes of the anisotropy, on the other hand, are only one third or less of those reported by the Tibet III experiment, indicating attenuation due to solar modulation. The rigidity dependence of the anisotropy amplitude in the sub-TeV region is consistent with the spectrum reported by Hall et al. (1999), smoothly extending to the Tibet III result in the multi-TeV region. The amplitude at higher energies appears almost constant or gradually decreasing with increasing rigidity.

K. Munakata; N. Matsumoto; S. Yasue; C. Kato; S. Mori; M. Takita; M. L. Duldig; J. E. Humble; J. Kota

2008-11-04T23:59:59.000Z

39

Intensity of Upward Muon Flux Due to Cosmic-Ray Neutrinos Produced in the Atmosphere  

DOE R&D Accomplishments (OSTI)

Calculations were performed to determine the upward going muon flux leaving the earth's surface after production by cosmic-ray neutrinos in the crust. Only neutrinos produced in the earth's atmosphere are considered. Rates of the order of one per 100 sq m/day might be expected if an intermediate boson exists and has a mass less than 2 Bev. (auth)

Lee, T. D.; Robinson, H.; Schwartz, M.; Cool, R.

1963-06-00T23:59:59.000Z

40

Luminosity Bias (II): The Cosmic Web of the First Stars  

E-Print Network (OSTI)

Understanding the formation and evolution of the first stars and galaxies represents one of the most exciting frontiers in astronomy. Since the universe was filled with neutral hydrogen at early times, the most promising method for observing the epoch of the first stars is using the prominent 21-cm spectral line of the hydrogen atom. Current observational efforts are focused on the reionization era (cosmic age t ~ 500 Myr), with earlier times considered much more challenging. However, the next frontier of even earlier galaxy formation (t ~ 200 Myr) is emerging as a promising observational target. This is made possible by a recently noticed effect of a significant relative velocity between the baryons and dark matter at early times. The velocity difference suppresses star formation, causing a unique form of early luminosity bias. The spatial variation of this suppression enhances large-scale clustering and produces a prominent cosmic web on 100 comoving Mpc scales in the 21-cm intensity distribution. This stru...

Barkana, Rennan

2013-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
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41

Fermilab | Science at Fermilab | Experiments & Projects | Experiments...  

NLE Websites -- All DOE Office Websites (Extended Search)

Particle Physics News Image Bank Fermilab in the News Quantum Diaries In this Section: Energy Frontier Intensity Frontier Cosmic Frontier Experiments at the Cosmic Frontier How...

42

Energy Frontier Research Centers  

NLE Websites -- All DOE Office Websites (Extended Search)

Frontier Research Centers Science for our Nation's Energy Future US Department of Energy Office of Science www.energyfrontier.us 43 ABOVE: CFSES addresses safe, secure and...

43

Fermilab | Science at Fermilab | Experiments & Projects  

NLE Websites -- All DOE Office Websites (Extended Search)

main content Science at Fermilab Frontiers of Particle Physics Experiments & Projects Energy Frontier Tevatron at Fermilab Fermilab and the LHC Intensity Frontier Cosmic Frontier...

44

Proton Accelerator Physics Continued| U.S. DOE Office of Science...  

Office of Science (SC) Website

Energy Frontier More Information High Energy Physics (HEP) HEP Home About Research Snowmass P5 Planning Process Energy Frontier Intensity Frontier Cosmic Frontier Theoretical...

45

Enabling Intensity and Energy Frontier Science with a Muon Accelerator Facility in the U.S.: A White Paper Submitted to the 2013 U.S. Community Summer Study of the Division of Particles and Fields of the American Physical Society  

E-Print Network (OSTI)

A staged approach towards muon based facilities for Intensity and Energy Frontier science, building upon existing and proposed facilities at Fermilab, is presented. At each stage, a facility exploring new physics also provides an R&D platform to validate the technology needed for subsequent stages. The envisioned program begins with nuSTORM, a sensitive sterile neutrino search which also provides precision neutrino cross-section measurements while developing the technology of using and cooling muons. A staged Neutrino Factory based upon Project X, sending beams towards the Sanford Underground Research Facility (SURF), which will house the LBNE detector, could follow for detailed exploration of neutrino properties at the Intensity Frontier, while also establishing the technology of using intense bunched muon beams. The complex could then evolve towards Muon Colliders, starting at 126 GeV with measurements of the Higgs resonance to sub-MeV precision, and continuing to multi-TeV colliders for the exploration of physics beyond the Standard Model at the Energy Frontier. An Appendix addresses specific questions raised by the Lepton Colliders subgroup of the CSS2013 Frontier Capabilities Study Group.

J-P. Delahaye; C. Ankenbrandt; A. Bogacz; S. Brice; A. Bross; D. Denisov; E. Eichten; P. Huber; D. M. Kaplan; H. Kirk; R. Lipton; D. Neuffer; M. A. Palmer; R. Palmer; R. Ryne; P. Snopok

2013-08-02T23:59:59.000Z

46

Instrumentation for the Energy Frontier  

E-Print Network (OSTI)

The Instrumentation Frontier was set up as a part of the Snowmass 2013 Community Summer Study to examine the instrumentation R&D needed to support particle physics research over the coming decade. This report summarizes the findings of the Energy Frontier subgroup of the Instrumentation Frontier.

Ulrich Heintz; Daniela Bortoletto; Marcus Hohlmann; Thomas LeCompte; Ron Lipton; Meenakshi Narain; Andrew White

2013-08-31T23:59:59.000Z

47

Diagnosis of an Intense Atmospheric River Impacting the Pacific Northwest: Storm Summary and Offshore Vertical Structure Observed with COSMIC Satellite Retrievals  

Science Conference Proceedings (OSTI)

This study uses the new satellite-based Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC) mission to retrieve tropospheric profiles of temperature and moisture over the data-sparse eastern Pacific Ocean. The COSMIC ...

Paul J. Neiman; F. Martin Ralph; Gary A. Wick; Ying-Hwa Kuo; Tae-Kwon Wee; Zaizhong Ma; George H. Taylor; Michael D. Dettinger

2008-11-01T23:59:59.000Z

48

The Climate Adaptation Frontier  

Science Conference Proceedings (OSTI)

Climate adaptation has emerged as a mainstream risk management strategy for assisting in maintaining socio-ecological systems within the boundaries of a safe operating space. Yet, there are limits to the ability of systems to adapt. Here, we introduce the concept of an adaptation frontier , which is defined as a socio-ecological system s transitional adaptive operating space between safe and unsafe domains. A number of driving forces are responsible for determining the sustainability of systems on the frontier. These include path dependence, adaptation/development deficits, values conflicts and discounting of future loss and damage. The cumulative implications of these driving forces are highly uncertain. Nevertheless, the fact that a broad range of systems already persist at the edge of their frontiers suggests a high likelihood that some limits will eventually be exceeded. The resulting system transformation is likely to manifest as anticipatory modification of management objectives or loss and damage. These outcomes vary significantly with respect to their ethical implications. Successful navigation of the adaptation frontier will necessitate new paradigms of risk governance to elicit knowledge that encourages reflexive reevaluation of societal values that enable or constrain sustainability.

Preston, Benjamin L [ORNL

2013-01-01T23:59:59.000Z

49

Fermilab | Science at Fermilab  

NLE Websites -- All DOE Office Websites (Extended Search)

to main content Science at Fermilab Frontiers of Particle Physics Experiments & Projects Energy Frontier Tevatron at Fermilab Fermilab and the LHC Intensity Frontier Cosmic...

50

Research | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Frontier Intensity Frontier Cosmic Frontier Theoretical Physics Advanced Technology R&D Accelerator R&D Stewardship Research Highlights .pdf file (13.1MB) Questions for the...

51

Connecting Accelerator RD to User Needs | U.S. DOE Office of...  

Office of Science (SC) Website

Connecting Accelerator R&D to User Needs High Energy Physics (HEP) HEP Home About Research Snowmass P5 Planning Process Energy Frontier Intensity Frontier Cosmic Frontier...

52

Non Accelerator Physics Continued| U.S. DOE Office of Science...  

Office of Science (SC) Website

Frontier Intensity Frontier Cosmic Frontier Theoretical Physics Advanced Technology R&D Accelerator R&D Stewardship Research Highlights .pdf file (13.1MB) Questions for the...

53

Background | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Frontier Intensity Frontier Cosmic Frontier Theoretical Physics Advanced Technology R&D Accelerator R&D Stewardship Mission Background HEP Accelerator R&D Expertise...

54

Computing Frontier: Distributed Computing  

NLE Websites -- All DOE Office Websites (Extended Search)

Computing Computing Frontier: Distributed Computing and Facility Infrastructures Conveners: Kenneth Bloom 1 , Richard Gerber 2 1 Department of Physics and Astronomy, University of Nebraska-Lincoln 2 National Energy Research Scientific Computing Center (NERSC), Lawrence Berkeley National Laboratory 1.1 Introduction The field of particle physics has become increasingly reliant on large-scale computing resources to address the challenges of analyzing large datasets, completing specialized computations and simulations, and allowing for wide-spread participation of large groups of researchers. For a variety of reasons, these resources have become more distributed over a large geographic area, and some resources are highly specialized computing machines. In this report for the Snowmass Computing Frontier Study, we consider several questions about distributed computing

55

SOLAR CYCLE DEPENDENCE OF THE DIURNAL ANISOTROPY OF 0.6 TeV COSMIC-RAY INTENSITY OBSERVED WITH THE MATSUSHIRO UNDERGROUND MUON DETECTOR  

SciTech Connect

We analyze the temporal variation of the diurnal anisotropy of sub-TeV cosmic-ray intensity observed with the Matsushiro (Japan) underground muon detector over two full solar activity cycles in 1985-2008. We find an anisotropy component in the solar diurnal anisotropy superimposed on the Compton-Getting anisotropy due to Earth's orbital motion around the Sun. The phase of this additional anisotropy is almost constant at {approx}15:00 local solar time corresponding to the direction perpendicular to the average interplanetary magnetic field at Earth's orbit, while the amplitude varies between a maximum (0.043% +- 0.002%) and minimum ({approx}0.008% +- 0.002%) in a clear correlation with the solar activity. We find a significant time lag between the temporal variations of the amplitude and the sunspot number (SSN) and obtain the best correlation coefficient of +0.74 with the SSN delayed for 26 months. We suggest that this anisotropy might be interpreted in terms of the energy change due to the solar-wind-induced electric field expected for galactic cosmic rays (GCRs) crossing the wavy neutral sheet. The average amplitude of the sidereal diurnal variation over the entire period is 0.034% +- 0.003%, which is roughly one-third of the amplitude reported from air shower and deep-underground muon experiments monitoring multi-TeV GCR intensity suggesting a significant attenuation of the anisotropy due to the solar modulation. We find, on the other hand, only a weak positive correlation between the sidereal diurnal anisotropy and the solar activity cycle in which the amplitude in the 'active' solar activity epoch is about twice the amplitude in the 'quiet' solar activity epoch. This implies that only one-fourth of the total attenuation varies in correlation with the solar activity cycle and/or the solar magnetic cycle. We finally examine the temporal variation of the 'single-band valley depth' (SBVD) quoted by the Milagro experiment and, in contrast with recent Milagro's report, we find no steady increase in the Matsushiro observations in a seven-year period between 2000 and 2007. We suggest, therefore, that the steady increase of the SBVD reported by the Milagro experiment is not caused by the decreasing solar modulation in the declining phase of the 23rd solar activity cycle.

Munakata, K.; Mizoguchi, Y.; Kato, C.; Yasue, S.; Mori, S. [Department of Physics, Shinshu University, Matsumoto 390-8621 (Japan); Takita, M. [Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582 (Japan); Kota, J., E-mail: kmuna00@shinshu-u.ac.j [Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 87721 (United States)

2010-04-01T23:59:59.000Z

56

Energy Frontier Research Centers | ORNL  

NLE Websites -- All DOE Office Websites (Extended Search)

Materials Synthesis from Atoms to Systems Materials Synthesis from Atoms to Systems Materials Characterization Materials Theory and Simulation Energy Frontier Research Centers Center for Defect Physics in Structural Materials Fluid Interface Reactions, Structure and Transport Advanced Materials Home | Science & Discovery | Advanced Materials | Research Areas | Energy Frontier Research Centers SHARE Energy Frontier Research Centers Advanced Materials research at ORNL is home to two Department of Energy-Office of Basic Energy Sciences' Energy Frontier Research Centers, the Fluid Interface Reaction, Structure, and Transport Center (FIRST), which focuses on understanding interfacial processes critical to electrical energy storage and catalysis, and the Center for Defect Physics, (CDP)

57

Grid Storage and the Energy Frontier Research Centers | Department...  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Grid Storage and the Energy Frontier Research Centers Grid Storage and the Energy Frontier Research Centers DOE: Grid Storage and the Energy Frontier Research Centers Grid Storage...

58

Frontier Associates | Open Energy Information  

Open Energy Info (EERE)

Frontier Associates Frontier Associates Jump to: navigation, search Name Frontier Associates Address 1515 S Capital of Texas Hwy Place Austin, Texas Zip 78746 Sector Efficiency Product Design, evaluation and implementation of energy efficiency, renewable energy, and pricing programs Website http://www.frontierassoc.com/ Coordinates 30.273701°, -97.816775° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":30.273701,"lon":-97.816775,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

59

Frontiers in High-Energy Astroparticle Physics  

E-Print Network (OSTI)

With the discovery of evidence for neutrino mass, a vivid gamma ray sky at multi-TeV energies, and cosmic ray particles with unexpectedly high energies, astroparticle physics currently runs through an era of rapid progress and moving frontiers. The non-vanishing neutrino mass establishes one smooth component of dark matter which does not, however, supply a critical mass to the Universe. Other dark matter particles are likely to be very massive and should produce high-energy gamma rays, neutrinos, and protons in annihilations or decays. The search for exotic relics with new gamma ray telescopes, extensive air shower arrays, and underwater/-ice neutrino telescopes is a fascinating challenge, but requires to understand the astrophysical background radiations at high energies. Among the high-energy sources in the Universe, radio-loud active galactic nuclei seem to be the most powerful accounting for at least a sizable fraction of the extragalactic gamma ray flux. They could also supply the bulk of the observed cosmic rays at ultrahigh energies and produce interesting event rates in neutrino telescopes aiming at the kubic kilometer scale such as AMANDA and ANTARES. It is proposed that the extragalactic neutrino beam can be used to search for tau lepton appearance thus allowing for a proof of the neutrino oscillation hypothesis. Furthermore, a new method for probing the era of star formation at high redshifts using gamma rays is presented which requires new-generation gamma ray telescopes operating in the 10-100 GeV regime such as MAGIC and GLAST.

Karl Mannheim

1999-02-12T23:59:59.000Z

60

Unique Aspects and Scientific Challenges - Advanced R and D|...  

Office of Science (SC) Website

Advanced R and D Unique Aspects and Scientific Challenges High Energy Physics (HEP) HEP Home About Research Snowmass P5 Planning Process Energy Frontier Intensity Frontier Cosmic...

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


61

Nanometric Optical Imaging Frontiers in Chemical Imaging  

E-Print Network (OSTI)

Nanometric Optical Imaging Frontiers in Chemical Imaging Seminar Series Presented by... Professor thermal imaging, chemical delivery and other new horizons. Finally, as part of this lecture, Lewis

62

Cosmic Parallax  

E-Print Network (OSTI)

Future satellite missions such as GAIA will achieve astrometry measurements with an accuracy of about 10 $\\mu$as for bright sources; other satellite proposals aim at 1 $\\mu$as. We show in this paper that such refined measurements allow us to detect large-scale deviations from isotropy through real-time observations of changes in the angular separation between sources at cosmic distances. We show that this "cosmic parallax'' effect is a powerful consistency test of Friedmann-Robertson-Walker metric and may set very strong constraints on alternative anisotropic models like Lemaitre-Tolman-Bondi cosmologies with off-center observers.

Quercellini, Claudia; Amendola, Luca

2008-01-01T23:59:59.000Z

63

Citations to Journal Articles from Energy Frontier Research Centers...  

Office of Scientific and Technical Information (OSTI)

Citations to Journal Articles from Energy Frontier Research Centers Now Available on OSTI's SciTech Connect Energy Frontier Research Centers map displaying 46 EFRCs in 35 states...

64

DOE to Award $100 Million for Energy Frontier Research Centers...  

Office of Science (SC) Website

DOE to Award 100 Million for Energy Frontier Research Centers Energy Frontier Research Centers (EFRCs) EFRCs Home Centers Research Science Highlights News & Events EFRC News EFRC...

65

Department of Energy Hosts Inaugural Energy Frontier Research...  

Office of Science (SC) Website

Department of Energy Hosts Inaugural Energy Frontier Research Center Summit Energy Frontier Research Centers (EFRCs) EFRCs Home Centers Research Science Highlights News & Events...

66

Quantum cryptography for security challenges to be topic of Frontiers...  

NLE Websites -- All DOE Office Websites (Extended Search)

Frontiers in Science lectures Quantum cryptography for security challenges to be topic of Frontiers in Science lectures Richard Hughes discusses the basics of cryptography and...

67

Frontiers in Chemical Imaging Seminar Series  

E-Print Network (OSTI)

Frontiers in Chemical Imaging Seminar Series X-ray Imaging at the Nanoscale Presented by Ian Mc and exquisite sensitivity to elemental, chemical and magnetic states in buried structures. The advent

68

Frontiers in Chemical Imaging Seminar Series  

E-Print Network (OSTI)

Frontiers in Chemical Imaging Seminar Series Advancing Methods for Labeling, Staining, Imaging is to understand how the interplay of structural, chemical and electrical signals in and between cells of nervous

69

Data-intensive e-science frontier research  

Science Conference Proceedings (OSTI)

Large-scale e-science, including high-energy and nuclear physics, biomedical informatics, and Earth science, depend on an increasingly integrated, distributed cyberinfrastructure serving virtual organizations on a global scale.

Harvey B. Newman; Mark H. Ellisman; John A. Orcutt

2003-11-01T23:59:59.000Z

70

Energy Frontier Research Center Events  

Office of Science (SC) Website

events/ The Office events/ The Office of Science is the single largest supporter of basic research in the physical sciences in the United States, providing more than 40 percent of total funding for this vital area of national importance. It oversees - and is the principal federal funding agency of - the Nation's research programs in high-energy physics, nuclear physics, and fusion energy sciences. en {7ED2520F-2DB2-435D-8CBE-DEC18A03F324}http://science.energy.gov/bes/efrc/news-and-events/efrc-events/princeton-cefrc-summer-program-on-combustion-2013-session/ Princeton-CEFRC Summer Program on Combustion: 2013 Session The Combustion Energy Frontier Research Center at Princeton University will host a summer program on Combustion. Mon, 11 Mar 2013 00:00:00 -0400 {0C172CD4-47D1-4231-A89B-7C7C4F0CA5E4}http://science.energy.gov/bes/efrc/news-and-events/efrc-events/approaches-to-ultrahigh-efficiency-solar-energy-conversion-webinar/

71

Quarkonium at the Frontiers of High Energy Physics: A Snowmass White Paper  

E-Print Network (OSTI)

In this Snowmass White Paper, we discuss physics opportunities involving heavy quarkonia at the intensity and energy frontiers of high energy physics. We focus primarily on two specific aspects of quarkonium physics for which significant advances can be expected from experiments at both frontiers. The first aspect is the spectroscopy of charmonium and bottomonium states above the open-heavy-flavor thresholds. Experiments at e^+ e^- colliders and at hadron colliders have discovered many new, unexpected quarkonium states in the last 10 years. Many of these states are surprisingly narrow, and some have electric charge. The observations of these charged quarkonium states are the first definitive discoveries of manifestly exotic hadrons. These results challenge our understanding of the QCD spectrum. The second aspect is the production of heavy quarkonium states with large transverse momentum. Experiments at the LHC are measuring quarkonium production with high statistics at unprecedented values of p_T. Recent theoretical developments may provide a rigorous theoretical framework for inclusive production of quarkonia at large p_T. Experiments at the energy frontier will provide definitive tests of this framework. Experiments at the intensity frontier also provide an opportunity to understand the exclusive production of quarkonium states.

Geoffrey T. Bodwin; Eric Braaten; Estia Eichten; Stephen Lars Olsen; Todd K. Pedlar; James Russ

2013-07-29T23:59:59.000Z

72

U.S. Department of Energy Announces Energy Frontier Research...  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Energy Frontier Research Centers Summit & Forum U.S. Department of Energy Announces Energy Frontier Research Centers Summit & Forum March 4, 2011 - 12:00am Addthis Washington, D.C....

73

Computing for the Energy Frontier: Snowmass Study 2013  

E-Print Network (OSTI)

The Contribution for the Computing for the Energy Frontier as part of the Snowmass study is discussed.

Fisk, Ian

2014-01-01T23:59:59.000Z

74

Computing for the Energy Frontier: Snowmass Study 2013  

E-Print Network (OSTI)

The Contribution for the Computing for the Energy Frontier as part of the Snowmass study is discussed.

Ian Fisk; Jim Shank

2014-01-08T23:59:59.000Z

75

Frontier Ethanol LLC | Open Energy Information  

Open Energy Info (EERE)

Frontier Ethanol LLC Frontier Ethanol LLC Jump to: navigation, search Name Frontier Ethanol LLC Place Gowrie, Iowa Product Owner and operator of a bioethanol plant near Gowrie, Iowa. Coordinates 42.28227°, -94.290334° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":42.28227,"lon":-94.290334,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

76

Frontiers in Chemical Imaging Seminar Series  

E-Print Network (OSTI)

Frontiers in Chemical Imaging Seminar Series Presented by Kannan M. Krishnan, Ph.D. Departments. Central to this work are innovations in chemical synthesis of nanoparticles, their size-dependent magnetic and technological interest, that may provide opportunities for future collaborative research in chemical imaging

77

Frontiers in thermoacoustic refrigeration and mixture separation  

E-Print Network (OSTI)

pulse-tube refrigerator shown in Figure 1 dissipates acoustic power by design because power must flowFrontiers in thermoacoustic refrigeration and mixture separation S. Backhaus1 , D. Geller2 , B oscillating thermodynamics in a gas in a sealed system. Since then, many related engines and refrigerators

78

Annual Report of the Institute for Frontier Medical Sciences Kyoto University  

E-Print Network (OSTI)

Annual Report of the Institute for Frontier Medical Sciences Kyoto University #12;#12;Institute for Frontier Medical Sciences 1 2 3 4 5 6 #12;#12;Institute for Frontier Medical Sciences 1 #12;Annual Report 2011 2 #12;Institute for Frontier Medical Sciences #12;Annual Report 2011 3 #12;Institute for Frontier

Takada, Shoji

79

Frontiers in Biological Sciences Seminar Series Presents Developing...  

NLE Websites -- All DOE Office Websites (Extended Search)

Frontiers in Biological Sciences Seminar Series Presents Developing Genome-Enabled Sustainable Lignocellulosic Biofuel Technologies at the Great Lakes Bioenergy Research Center...

80

Three Frontiers in the Thermodynamics of Protein Solutions  

E-Print Network (OSTI)

Three frontiers in the thermodynamics of protein solutions*the broad high- way of thermodynamics. ” ACKNOWLEDGMENTS ForThe great virtue of thermodynamics is its generality, its

Prausnitz, John M; Foose, Loddie

2007-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


81

Three Frontiers in the Thermodynamics of Protein Solutions  

E-Print Network (OSTI)

is the broad highway of thermodynamics. Acknowledgments: ForThree Frontiers in the Thermodynamics of Protein SolutionsThe great virtue of thermodynamics is its generality, its

Prausnitz, John; Hagar, Loddie

2008-01-01T23:59:59.000Z

82

High Energy Cosmic Rays  

E-Print Network (OSTI)

.Hebbeker Radiation Exposure of Humans Natural sources: ~ 1 m Sv / year ~ 1 m Gy / year ~ 0,1 J / year Technical sources: ~ 1 m Sv / Jahr ~ natural exposure Air (Radon) internal radioactivity (K-40) cosmics Increased of Cosmic Radiation Nobel 1936 1912 Viktor Hess 1912 #12;T.Hebbeker Electrometer Measurements V. Hess

Hebbeker, Thomas

83

Life at the Frontiers of Energy Research Video Contest | U.S...  

Office of Science (SC) Website

Life at the Frontiers of Energy Research Video Contest Energy Frontier Research Centers (EFRCs) EFRCs Home Centers Research Science Highlights News & Events EFRC News EFRC Events...

84

Light from cosmic strings  

Science Conference Proceedings (OSTI)

The time-dependent metric of a cosmic string leads to an effective interaction between the string and photons--the ''gravitational Aharonov-Bohm'' effect--and causes cosmic strings to emit light. We evaluate the radiation of pairs of photons from cosmic strings and find that the emission from cusps, kinks and kink-kink collisions occurs with a flat spectrum at all frequencies up to the string scale. Further, cusps emit a beam of photons, kinks emit along a curve, and the emission at a kink-kink collision is in all directions. The emission of light from cosmic strings could provide an important new observational signature of cosmic strings that is within reach of current experiments for a range of string tensions.

Steer, Daniele A.; Vachaspati, Tanmay [APC 10 rue Alice Domon et Leonie Duquet, 75205 Paris Cedex 13 (France); Physics Department, Arizona State University, Tempe, Arizona 85287 (United States)

2011-02-15T23:59:59.000Z

85

Department of Energy to Host Inaugural Energy Frontier Research Center  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

to Host Inaugural Energy Frontier Research to Host Inaugural Energy Frontier Research Center Summit Department of Energy to Host Inaugural Energy Frontier Research Center Summit May 24, 2011 - 12:00am Addthis WASHINGTON, D.C. - On Wednesday, May 25, U.S. Department of Energy Secretary Steven Chu will welcome nearly 1,000 of America's top energy researchers to Washington, D.C. for the inaugural Science for the Nation's Energy Future: The Energy Frontier Research Centers Summit and Forum. The three-day public conference will showcase early successes of DOE's Energy Frontier Research Centers (EFRC). It will also bring together scientists and energy policy leaders to explore the challenges and opportunities in applying America's extraordinary scientific and technical resources to helping shape our clean energy future.

86

Electron Ion Collider: The Next QCD Frontier  

NLE Websites -- All DOE Office Websites (Extended Search)

Ion Collider: Ion Collider: The Next QCD Frontier Understanding the glue that binds us all Electron Ion Collider: The Next QCD Frontier Understanding the glue that binds us all BNL-98815-2012-JA JLAB-PHY-12-1652 arXiv:1212.1701 Authors A. Accardi 14,28 , J. L. Albacete 16 , M. Anselmino 29 , N. Armesto 36 , E. C. Aschenauer 3,† , A. Bacchetta 35 , D. Boer 33 , W. Brooks 37,† , T. Burton 3 , N.-B. Chang 23 , W.-T. Deng 13,23 , A. Deshpande 25,∗,† , M. Diehl 11,† , A. Dumitru 2 , R. Dupr´ e 7 , R. Ent 28,‡ , S. Fazio 3 , H. Gao 12,† , V. Guzey 28 , H. Hakobyan 37 , Y. Hao 3 , D. Hasch 15 , R. Holt 1,† , T. Horn 5,† , M. Huang 23 , A. Hutton 28,† , C. Hyde 20 , J. Jalilian-Marian 2 , S. Klein 17 , B. Kopeliovich 37 , Y. Kovchegov 19,† , K. Kumar 24,† , K. Kumeriˇ cki 40 , M. A. C. Lamont 3 , T. Lappi 34 , J.-H. Lee 3 , Y. Lee 3 , E. M. Levin 26,37 , F.-L. Lin 28 , V. Litvinenko 3 , T. W. Ludlam 3,‡ , C. Marquet

87

Influence of solar and cosmic-ray variability on climate  

E-Print Network (OSTI)

We analyze solar, geomagnetic and cosmic ray flux data along with rainfall and temperature data for almost five solar cycles. We provide evidence of significant influence of solar variability on climate. Specifically, we demonstrate association between lower (higher) rainfall and higher (lower) temperatures with increasing (decreasing) solar activity and decreasing (increasing) cosmic ray intensities. We propose a plausible scenario that accounts the results of our analysis.

Badruddin,; Singh, M

2013-01-01T23:59:59.000Z

88

Cosmic Microwave Background Project at NERSC  

NLE Websites -- All DOE Office Websites (Extended Search)

Cosmic Microwave Background Cosmic Microwave Background CMB.jpg The Cosmic Microwave Background (CMB) is relic radiation from a very early stage in the universe -- essentially a...

89

The Cosmic Energy Inventory  

E-Print Network (OSTI)

We present an inventory of the cosmic mean densities of energy associated with all the known states of matter and radiation at the present epoch. The observational and theoretical bases for the inventory have become rich enough to allow estimates with observational support for the densities of energy in some 40 forms. The result is a global portrait of the effects of the physical processes of cosmic evolution.

Masataka Fukugita; P. J. E. Peebles

2004-06-03T23:59:59.000Z

90

Development of a Low-Energy Proton Accelerator System for the Proton Engineering Frontier Project (PEFP)  

E-Print Network (OSTI)

Development of a Low-Energy Proton Accelerator System for the Proton Engineering Frontier Project (PEFP)

Han, J M

2003-01-01T23:59:59.000Z

91

Contruction of User Facilities for the Proton Beam Utilization of PEFP (Proton Engineering Frontier Project)  

E-Print Network (OSTI)

Contruction of User Facilities for the Proton Beam Utilization of PEFP (Proton Engineering Frontier Project)

Kim, K R; Lee, H R; Nam, K Y; Park, B S

2003-01-01T23:59:59.000Z

92

Frontier Power Company | Open Energy Information  

Open Energy Info (EERE)

Power Company Power Company Place Ohio Utility Id 6804 Utility Location Yes Ownership C NERC Location RFC NERC RFC Yes RTO PJM Yes Activity Transmission Yes Activity Distribution Yes References EIA Form EIA-861 Final Data File for 2010 - File1_a[1] LinkedIn Connections CrunchBase Profile No CrunchBase profile. Create one now! This article is a stub. You can help OpenEI by expanding it. Utility Rate Schedules Grid-background.png Commercial And Industrial Lighting And Power Service Commercial Large Power Service Residential Sales,Residential Sales Seasonal And Public Building Service Residential Average Rates Residential: $0.1160/kWh Commercial: $0.1180/kWh References ↑ "EIA Form EIA-861 Final Data File for 2010 - File1_a" Retrieved from "http://en.openei.org/w/index.php?title=Frontier_Power_Company&oldid=410728"

93

IGNITION AND FRONTIER SCIENCE ON THE NATIONAL IGNITION FACILITY  

Science Conference Proceedings (OSTI)

The National Ignition Facility (NIF), the world's largest and most powerful laser system for inertial confinement fusion (ICF) and experiments studying high-energy-density (HED) science, is now operational at Lawrence Livermore National Laboratory (LLNL). The NIF construction Project was certified by the Department of Energy as complete on March 30, 2009. NIF, a 192-beam Nd-glass laser facility, will produce 1.8 MJ, 500 TW of light at the third-harmonic, ultraviolet light of 351 nm. On March 10, 2009, a total 192-beam energy of 1.1 MJ was demonstrated; this is approximately 30 times more energy than ever produced in an ICF laser system. The principal goal of NIF is to achieve ignition of a deuterium-tritium (DT) fuel capsule and provide access to HED physics regimes needed for experiments related to national security, fusion energy and for broader frontier scientific exploration. NIF experiments in support of indirect drive ignition will begin in FY2009. These first experiments represent the next phase of the National Ignition Campaign (NIC). The NIC is a 1.7 billion dollar national effort to achieve fusion ignition and is coordinated through a detailed execution plan that includes the science, technology, and equipment. Equipment required for ignition experiments include diagnostics, cryogenic target manipulator, and user optics. Participants in this effort include LLNL, General Atomics (GA), Los Alamos National Laboratory (LANL), Sandia National Laboratory (SNL), and the University of Rochester Laboratory for Energetics (LLE). The primary goal for NIC is to have all of the equipment operational and integrated into the facility and be ready to begin a credible ignition campaign in 2010. With NIF now operational, the long-sought goal of achieving self-sustained nuclear fusion and energy gain in the laboratory is much closer to realization. Successful demonstration of ignition and net energy gain on NIF will be a major step towards demonstrating the feasibility of Inertial Fusion Energy (IFE) and will likely focus the world's attention on the possibility of an ICF energy option. NIF experiments to demonstrate ignition and gain will use central-hot-spot (CHS) ignition, where a spherical fuel capsule is simultaneously compressed and ignited. The scientific basis for CHS has been intensively developed and has high probability of success. Achieving ignition with CHS will open the door for other advanced concepts, such as the use of high-yield pulses of visible wavelength rather than ultraviolet and Fast Ignition concepts. Moreover, NIF will have important scientific applications in such diverse fields as astrophysics, nuclear physics and materials science. The NIC will develop the full set of capabilities required to operate NIF as a major national and international user facility. A solicitation for NIF frontier science experiments to be conducted by the academic community is planned for summer 2009. This paper summarizes the design, performance, and status of NIF, experimental plans for NIC, and will present a brief discussion of the unparalleled opportunities to explore frontier basic science that will be available on the NIF.

Moses, E

2009-06-22T23:59:59.000Z

94

Basin analog approach answers characterization challenges of unconventional gas potential in frontier basins  

E-Print Network (OSTI)

To continue increasing the energy supply to meet global demand in the coming decades, the energy industry needs creative thinking that leads to the development of new energy sources. Unconventional gas resources, especially those in frontier basins, will play an important role in fulfilling future world energy needs. We must identify and quantify potential unconventional gas resources in basins around the world to plan for their development. Basin analog assessment is one technique that can be used to identify and quantify unconventional gas resources that is less expensive and less time consuming. We have developed a basin analog methodology that is useful for rapidly and consistently evaluating the unconventional hydrocarbon resource potential in exploratory basins. We developed software, Basin Analog System (BAS), to perform and accelerate the process of identifying analog basins. Also, we built a database that includes geologic and petroleum systems information of intensely studied North America basins that contain well characterized conventional and unconventional hydrocarbon resources. We have selected 25 basins in North America that have a history of producing unconventional gas resources. These are �reference� basins that are used to predict resources in frontier or exploratory basins. The software assists us in ranking reference basins that are most analogous to the target basin for the primary purpose of evaluating the potential unconventional resources in the target basin. The methodology allows us to numerically rank all the reference basins relative to the target basin. The accuracy of the results depends on the descriptions of geologic and petroleum systems. We validated the software to make sure it is functioning correctly and to test the validity of the process and the database. Finding a reference basin that is analogous to a frontier basin can provide insights into potential unconventional gas resources of the frontier basin. Our method will help industry predict the unconventional hydrocarbon resource potential of frontier basins, guide exploration strategy, infer reservoir characteristics, and make preliminary decisions concerning the best engineering practices as wells are drilled, completed, stimulated and produced.

Singh, Kalwant

2006-12-01T23:59:59.000Z

95

Energy Department to Award $100 Million for Energy Frontier Research  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

to Award $100 Million for Energy Frontier to Award $100 Million for Energy Frontier Research Centers Energy Department to Award $100 Million for Energy Frontier Research Centers September 30, 2013 - 4:39pm Addthis NEWS MEDIA CONTACT (202) 586-4940 WASHINGTON - U.S. Energy Secretary Ernest Moniz today announced a proposed $100 million in FY2014 funding for Energy Frontier Research Centers to accelerate the scientific breakthroughs needed to build a new 21st-century energy economy. Research supported by this initiative will enable fundamental advances in energy production and use. "Transforming how we generate, transmit, store and use energy is one of the greatest scientific challenges we face in the changing energy landscape," said Secretary Moniz. "This funding will help fuel innovative solutions as we move toward next generation energy systems."

96

Frontiers in Science Lectures focus on saving energy through  

NLE Websites -- All DOE Office Websites (Extended Search)

Frontiers in Science Lectures Frontiers in Science Lectures Frontiers in Science Lectures focus on saving energy through superconductivity Dean Peterson discusses the science of high-temperature superconductivity in a series of Frontiers in Science lectures. June 12, 2009 Los Alamos National Laboratory sits on top of a once-remote mesa in northern New Mexico with the Jemez mountains as a backdrop to research and innovation covering multi-disciplines from bioscience, sustainable energy sources, to plasma physics and new materials. Los Alamos National Laboratory sits on top of a once-remote mesa in northern New Mexico with the Jemez mountains as a backdrop to research and innovation covering multi-disciplines from bioscience, sustainable energy sources, to plasma physics and new materials.

97

Frontiers in Chemical Physics and Analysis Seminar Series  

E-Print Network (OSTI)

Frontiers in Chemical Physics and Analysis Seminar Series Aqueous Solvation in Extreme Conditions the application of classical chemical dynamics simulations possible for a broad range of problems. However, since

98

Director Charlie McMillan presents the new supercomputer frontier  

NLE Websites -- All DOE Office Websites (Extended Search)

of our computers to do our mission. The ongoing weapon life-extension programs and our annual assessment of the deterrent depend on it. This means a new frontier in supercomputing,...

99

Fifth German-American Frontiers of Engineering Symposium  

SciTech Connect

The agenda book for the Fifth German-American Frontiers of Engineering Symposium contains abstracts of the 16 presentations as well as information on the program, bios of the speakers, contact information for all attendees, and background on the activity.

2002-05-01T23:59:59.000Z

100

Department of Energy to Host Energy Frontier Research Center Summit |  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

to Host Energy Frontier Research Center Summit to Host Energy Frontier Research Center Summit Department of Energy to Host Energy Frontier Research Center Summit May 24, 2011 - 12:00am Addthis Washington, DC - Beginning Wednesday, May 25 U.S. Secretary of Energy Steven Chu will welcome nearly 1,000 of America's top energy researchers to Washington, D.C. for the inaugural Science for the Nation's Energy Future: The Energy Frontier Research Centers Summit and Forum. The three-day event will bring together scientists and energy policy leaders to explore the challenges and opportunities in applying America's extraordinary scientific and technical resources to helping shape our clean energy future. Secretary Chu will give the opening keynote address on Wednesday, May 25 and discuss how technology and innovation can help solve the nation's energy needs.

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


101

DOE to establish two Energy Frontier Research Centers at Argonne...  

NLE Websites -- All DOE Office Websites (Extended Search)

Energy's (DOE) Argonne National Laboratory will be home to two of 46 new multi-million-dollar Energy Frontier Research Centers (EFRCs) announced today by the White House in...

102

Heart of the Solution - Energy Frontiers (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'Heart of the Solution - Energy Frontiers' was submitted by the Center for Solar and Thermal Energy Conversion (CSTEC) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. This video was both the People's Choice Award winner and selected as one of five winners by a distinguished panel of judges for its 'exemplary explanation of the role of an Energy Frontier Research Center'. The Center for Solar and Thermal Energy Conversion is directed by Peter F. Green at the University of Michigan. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of the Center for Solar and Thermal Energy Conversion is 'to study complex material structures on the nanoscale to identify key features for their potential use as materials to convert solar energy and heat to electricity.' Research topics are: solar photovoltaic, photonic, optics, solar thermal, thermoelectric, phonons, thermal conductivity, solar electrodes, defects, ultrafast physics, interfacial characterization, matter by design, novel materials synthesis, charge transport, and self-assembly.

Green, Peter F. (Director, Center for Solar and Thermal Energy Conversion, University of Michigan); CSTEC Staff

2011-05-01T23:59:59.000Z

103

HEP Early Career Research Opportunities | U.S. DOE Office of...  

Office of Science (SC) Website

Essig, Rouven Stony Brook University Stony Brook, NY Particle Physics at the Cosmic Intensity, and Energy Frontiers Hartnoll, Sean Stanford University Palo Alto, CA...

104

Ultrahigh Energy Cosmic Rays Detection  

Science Conference Proceedings (OSTI)

The paper describes methods used for the detection of cosmic rays with energies above 1018 eV (UHECR

Carla Aramo

2005-01-01T23:59:59.000Z

105

A disintegrating cosmic string  

E-Print Network (OSTI)

We present a simple sandwich gravitational wave of the Robinson-Trautman family. This is interpreted as representing a shock wave with a spherical wavefront which propagates into a Minkowski background minus a wedge. (i.e. the background contains a cosmic string.) The deficit angle (the tension) of the string decreases through the gravitational wave, which then ceases. This leaves an expanding spherical region of Minkowski space behind it. The decay of the cosmic string over a finite interval of retarded time may be considered to generate the gravitational wave.

J. B. Griffiths; P. Docherty

2002-04-29T23:59:59.000Z

106

The Amazon Frontier of Land-Use Change: Croplands and Consequences for Greenhouse Gas Emissions  

Science Conference Proceedings (OSTI)

The Brazilian Amazon is one of the most rapidly developing agricultural frontiers in the world. The authors assess changes in cropland area and the intensification of cropping in the Brazilian agricultural frontier state of Mato Grosso using ...

Gillian L. Galford; Jerry Melillo; John F. Mustard; Carlos E. P. Cerri; Carlos C. Cerri

2010-10-01T23:59:59.000Z

107

Cosmic Ray Telescopes  

NLE Websites -- All DOE Office Websites (Extended Search)

Cosmic Ray Muon Detectors Cosmic Ray Muon Detectors Particle Physics Using Nature's Accelerator Somewhere out there is a list of "10 Things a Physics Teacher is Least Likely to Say." If one were to find this list, it would have on it such gems as #7. Let's challenge the PE Dept to a game of rugby and #4. I don't care if you understand the concept, just give me the correct answer to 12 sig figs. Finally, you'd get down to the biggie, the thing physics teachers never say: #1. Let's do a particle physics lab right here at Podunk Corners High! The traditional reasons for this are that everyone knows that particle physics is only done with Vastly Expensive and Complicated Equipment run by casts of thousands of Highly Qualified Scientists and that particle physics is Difficult and Arcane.

108

Stable Charged Cosmic Strings  

Science Conference Proceedings (OSTI)

We study the quantum stabilization of a cosmic string by a heavy fermion doublet in a reduced version of the standard model. We show that charged strings, obtained by populating fermionic bound state levels, become stable if the electroweak bosons are coupled to a fermion that is less than twice as heavy as the top quark. This result suggests that extraordinarily large fermion masses or unrealistic couplings are not required to bind a cosmic string in the standard model. Numerically we find the most favorable string profile to be a simple trough in the Higgs vacuum expectation value of radius {approx_equal}10{sup -18} m. The vacuum remains stable in our model, because neutral strings are not energetically favored.

Weigel, H. [Physics Department, Stellenbosch University, Matieland 7602 (South Africa); Quandt, M. [Institute for Theoretical Physics, Tuebingen University, D-72076 Tuebingen (Germany); Graham, N. [Department of Physics, Middlebury College , Middlebury, Vermont 05753 (United States)

2011-03-11T23:59:59.000Z

109

New Frontiers in Energy Summit | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

New Frontiers in Energy Summit New Frontiers in Energy Summit New Frontiers in Energy Summit March 28, 2008 - 11:49am Addthis Remarks by Secretary Bodman Thank you, Sen. Salazar. I appreciate your strong commitment to helping this state - and our nation - address our energy challenges in a way that is comprehensive and sustainable for the long-term. In particular, you've been a real leader on renewable energy - through your work on the Senate Energy Committee - and I look forward to continuing to work with you back in Washington. It is indeed a pleasure to be in the great state of Colorado. This state is blessed with tremendous natural beauty - and vast natural resources -- resources which make Colorado a treasured haven for outdoor enthusiasts and which make the people who live here so strongly committed to protecting and

110

New Frontiers in Energy Summit | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

New Frontiers in Energy Summit New Frontiers in Energy Summit New Frontiers in Energy Summit March 28, 2008 - 11:49am Addthis Remarks by Secretary Bodman Thank you, Sen. Salazar. I appreciate your strong commitment to helping this state - and our nation - address our energy challenges in a way that is comprehensive and sustainable for the long-term. In particular, you've been a real leader on renewable energy - through your work on the Senate Energy Committee - and I look forward to continuing to work with you back in Washington. It is indeed a pleasure to be in the great state of Colorado. This state is blessed with tremendous natural beauty - and vast natural resources -- resources which make Colorado a treasured haven for outdoor enthusiasts and which make the people who live here so strongly committed to protecting and

111

U.S. DOE Energy Frontier Research Center Announcements  

Office of Science (SC) Website

doe-announcements/ The doe-announcements/ The Office of Science is the single largest supporter of basic research in the physical sciences in the United States, providing more than 40 percent of total funding for this vital area of national importance. It oversees - and is the principal federal funding agency of - the Nation's research programs in high-energy physics, nuclear physics, and fusion energy sciences. en {2FC67298-672C-476B-B645-000DED9B5398}http://science.energy.gov/bes/efrc/news-and-events/doe-announcements/doe-to-award-$100-million-for-energy-frontier-research-centers/ DOE to Award $100 Million for Energy Frontier Research Centers U.S. Energy Secretary Ernest Moniz today announced a proposed $100 million in FY2014 funding for Energy Frontier Research Centers to accelerate the scientific

112

Lab's Frontiers in Science lectures focus on epigenetics  

NLE Websites -- All DOE Office Websites (Extended Search)

Frontiers in Science lectures focus on epigenetics Frontiers in Science lectures focus on epigenetics Lab's Frontiers in Science lectures focus on epigenetics Sanbonmatsu will discuss the new science of epigenetics and how it is related to a wide range of biological phenomena. August 7, 2013 Cells in the human body contains strands of DNA nearly 10 feet long that look like this and are packed into cellular sacks less than a millionth of an inch in diameter. Cells in the human body contains strands of DNA nearly 10 feet long that look like this and are packed into cellular sacks less than a millionth of an inch in diameter. Contact Steve Sandoval Communications Office (505) 665-9206 Email Nick Njegomir Communications Office (505) 667-7000 Email "The act of a mother nurturing or not nurturing her baby programs DNA; so

113

US Residential Energy Demand and Energy Efficiency: A Stochastic Demand Frontier  

E-Print Network (OSTI)

US Residential Energy Demand and Energy Efficiency: A Stochastic Demand Frontier Approach Massimo www.cepe.ethz.ch #12;US Residential Energy Demand and Energy Efficiency: A Stochastic Demand Frontier Approach Page 1 of 25 US Residential Energy Demand and Energy Efficiency: A Stochastic Demand Frontier

114

cosmicfrontiermoreinfo | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Cosmic Frontier: More Information Cosmic Frontier: More Information High Energy Physics (HEP) HEP Home About Research Snowmass / P5 Planning Process Intensity Frontier Cosmic Frontier Cosmic Frontier: More Information Unique Aspects and Scientific Challenges Theoretical Physics Advanced Technology R&D Accelerator R&D Stewardship Research Highlights .pdf file (13.1MB) Questions for the Universe Accomplishments Facilities Science Highlights Benefits of HEP Funding Opportunities Advisory Committees News & Resources Contact Information High Energy Physics U.S. Department of Energy SC-25/Germantown Building 1000 Independence Ave., SW Washington, DC 20585 P: (301) 903-3624 F: (301) 903-2597 E: sc.hep@science.doe.gov More Information » Cosmic Frontier Cosmic Frontier: More Information Print Text Size: A A A

115

Cosmic Growth History and Expansion History  

E-Print Network (OSTI)

LBNL- 58260 Cosmic Growth History andExpansion History Eric V. Linder Physics Division, LawrenceCalifornia. Cosmic Growth History and Expansion History Eric

Linder, Eric V.

2009-01-01T23:59:59.000Z

116

POLARIZATION OF THE COSMIC BACKGROUND RADIATION  

E-Print Network (OSTI)

Galactic Synchrotron Radiation at 33 GHz NOIiWNPQaa s x s sthe Cosmic Background Radiation Philip Michael Lubin Spacethe Cosmic Background Radiation. The ground-based experiment

Lubin, Philip Lubin

2010-01-01T23:59:59.000Z

117

McKinsey Global Institute Big data: The next frontier  

E-Print Network (OSTI)

McKinsey Global Institute Big data: The next frontier for innovation, competition, and productivity June 2011 #12;The McKinsey Global Institute The McKinsey Global Institute (MGI), established in 1990, is McKinsey & Company's business and economics research arm. MGI's mission is to help leaders

Chen, Keh-Hsun

118

The Role of XAFS in Advancing the Frontiers of Molecular  

E-Print Network (OSTI)

The Role of XAFS in Advancing the Frontiers of Molecular Environmental Science Donald L. Sparks S information on the molecular aspects and interactions of a compounds No direct electronic information Magnetic under high vacuum (ex-situ) #12;#12;Molecular Environmental Science Study of the chemical and physical

Sparks, Donald L.

119

Burning Plasma Physics -The Next Frontier Three Options  

E-Print Network (OSTI)

Burning Plasma Physics - The Next Frontier Three Options (same scale) ITER-FEATFIRE IGNITOR US in Magnetic Fusion · Burning Plasma Performance Considerations · Compact High Field Approach - General for strengthening the base fusion sciences program 2. Directs DOE to submit a plan for a U.S. Burning Plasma

120

Cosmic Strings in Supergravity  

E-Print Network (OSTI)

It is pointed out that various types of cosmic string solutions that exist in nonsupersymmetric and globally supersymmetric theories, such as D-type gauge strings, F-type global and gauge strings, and superconducting Witten strings, also exist in supergravity models. When the D term and superpotential satisfy some simple conditions allowing the determination of a set of vacuum states with nontrivial topology, the existence of a string embedded within a supersymmetric vacuum with vanishing cosmological constant can be inferred. Supergravity also admits other string solutions, some of which have no counterparts in globally supersymmetric theories.

J. R. Morris

1997-06-09T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


121

Signatures of Cosmic Strings in the Cosmic Microwave Background  

E-Print Network (OSTI)

We report a search for signatures of cosmic strings in the the Cosmic Microwave Background data from the Wilkinson Microwave Anisotropy Probe. We used a digital filter designed to search for individual cosmic strings and found no evidence for them in the WMAP CMB anisotropies to a level of $\\Delta T/T \\sim 0.29$ mK. This corresponds to an absence of cosmic strings with $ G\\mu \\ga 1.07 \\times 10^{-5}$ for strings moving with velocity $v = c/\\sqrt{2}$. Unlike previous work, this limit does not depend on an assumed string abundance. We have searched the WMAP data for evidence of a cosmic string recently reported as the CSL-1 object, and found an ``edge'' with 2$\\sigma$ significance. However, if this edge is real and produced by a cosmic string, it would have to move at velocity $\\ga$ 0.94c. We also present preliminary limits on the CMB data that will be returned by the PLANCK satellite for comparison. With the available information on the PLANCK satellite, we calculated that it would be twice as sensitive to cosmic strings as WMAP.

Amy S. Lo; Edward L. Wright

2005-03-05T23:59:59.000Z

122

Fermilab | Science at Fermilab | Experiments & Projects | Intensity  

NLE Websites -- All DOE Office Websites (Extended Search)

Intensity Frontier Intensity Frontier MiniBooNE Researchers initiated the Booster Neutrino Experiment, BooNE, to verify definitively the results of the Los Alamos Liquid Scintillator Neutrino Detector experiment. In 1995, the Los Alamos experiment presented strong evidence for the oscillation of muon anti-neutrinos into electron anti-neutrinos. Jasmine Ma inspects one of the phototubes that detects light from neutrino interactions. (Courtesy: Peter Ginter) Jasmine Ma inspects one of the phototubes that detects light from neutrino interactions. (Courtesy: Peter Ginter) The 800-ton detector, called MiniBooNE, searches for neutrino oscillations. The detector is located 500 meters from Fermilab's second neutrino source, the Booster Neutrino Beam or BNB. The presence of neutrinos can only be inferred by detecting the charged

123

PNNL: Biological Sciences: Frontiers in Biological Sciences Seminar Series  

NLE Websites -- All DOE Office Websites (Extended Search)

Frontiers in Biological Sciences Frontiers in Biological Sciences The seminar series features nationally/internationally known researchers from industry, government, and academia discussing novel ideas and advancements related to biological sciences. The hour-long seminars will feature a 45-minute talk by the featured speaker followed by 15 minutes of discussion with the audience members. 2014 Tim Donohue Timothy J. Donohue, Ph.D. Timothy J. Donohue, Ph.D. Department of Bacteriology University of Wisconsin-Madison Director, Great Lakes Bioenergy Research Center Tuesday, January 14, 2014 EMSL Auditorium 11:00 a.m. Biological Insights and Products Gleaned from Mining Bacterial Genomes and Pathways Professor Donohue has been a member of the UW-Madison Bacteriology Department since 1986. His research program studies bacterial energy

124

PNNL: Atmospheric Sciences & Global Change - Frontiers in Global Change  

NLE Websites -- All DOE Office Websites (Extended Search)

Frontiers in Global Change Frontiers in Global Change Dr. Thanos Nenes Dr. Thanos Nenes Aerosol-Cloud Interactions: The Elusive Component of Climate Change Dr. Thanos Nenes Professor & Georgia Power Faculty Scholar, School of Earth & Atmospheric Sciences, School of Chemical & Biomolecular Engineering, Georgia Institute of Technology, Atlanta, GA Thursday, August 1, 2013 EMSL Auditorium 10:00AM The effect of human activities on climate is one of the most important issues facing society. Humans influence climate in many ways. Emissions of greenhouse gases (GHGs) tend to warm climate, by reducing the amount of infrared radiation that is emitted to space. Increased levels of suspended atmospheric particles ("aerosols") exert a net cooling effect by directly scattering and absorption of solar radiation (the "aerosol direct climatic

125

Frontier, North Dakota: Energy Resources | Open Energy Information  

Open Energy Info (EERE)

Frontier, North Dakota: Energy Resources Frontier, North Dakota: Energy Resources Jump to: navigation, search Equivalent URI DBpedia Coordinates 46.8005206°, -96.8331391° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":46.8005206,"lon":-96.8331391,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

126

Institute for Atom-Efficient Chemical Transformations Energy Frontier  

NLE Websites -- All DOE Office Websites (Extended Search)

Institute for Atom-Efficient Chemical Transformations DOE Logo Institute for Atom-Efficient Chemical Transformations DOE Logo Focus Areas Reaction Mechanisms Controlled Active Metals Materials Synthesis Search Argonne ... Search Argonne Home > Institute for Atom-Efficient Chemical Transformations > IACT Home IACT News IACT Partners IACT Staff IACT Awards Publications & Presentations Jobs at IACT Energy Frontier Research Centers at Argonne Strategic Alliances Research Facilities & Tools Institute for Atom-Efficient Chemical Transformations - an Energy Frontier Research Center The Institute for Atom-Efficient Chemical Transformations (IACT) employs a multidisciplinary approach to address key catalytic conversions that could improve the efficiency of producing fuels from biomass. IACT focuses on advancing the science of catalysis for the efficient conversion of energy resources into usable forms. IACT's goal is to find ways to achieve control and efficiency of chemical conversions comparable to those in nature.

127

FRONTIER SYNCHROTRON INFRARED SPECTROSCOPY BEAMLINE UNDER EXTREME CONDITIONS (FIS)  

NLE Websites -- All DOE Office Websites (Extended Search)

FRONTIER SYNCHROTRON INFRARED SPECTROSCOPY FRONTIER SYNCHROTRON INFRARED SPECTROSCOPY BEAMLINE UNDER EXTREME CONDITIONS (FIS) Proposal Team: L. Carr 1 , D. Dolan 2 , R. Hemley 3 , S. Jacobson 4 , S. Karato 5 , Z. Liu 3 , W. Panero 6 , M. Pravica 7 , and T. Zhou 8 1 Brookhaven National Laboratory, 2 Sandia National Laboratories, 3 Carnegie Institution of Washington, 4 Northwestern University, 5 Yale University, 6 Ohio State University, 7 University of Nevada, 8 New Jersey Institute of Technology TECHNIQUES AND CAPABILITIES APPLICATIONS SPECIFIC PROJECTS / ADDITIONAL INFORMATION * TECHNIQUE(S): Fourier transform infrared spectroscopy; Raman and visible spectroscopy; Diamond anvil cell techniques for static high pressure; Gas-gun launchers for dynamic compression; Cryogenic techniques combined with DACs;

128

Frontiers in X-Ray Science  

Science Conference Proceedings (OSTI)

The year 2010 marked the fiftieth anniversary of the optical laser and the first anniversary of the world's first hard x-ray free-electron laser, the Linac Coherent Light Source (LCLS) at SLAC. This exciting, new accelerator-based source of x-rays provides peak brilliances roughly a billion times greater than currently available from synchrotron sources such as the Advanced Photon Source at Argonne, and thus explores a qualitatively different parameter space. This talk will describe the first experiments at the LCLS aimed at understanding the nature of high intensity x-ray interactions, related applications in ultrafast imaging on the atomic scale and sketch nascent plans for the extension of both linac and storage-ring based photon sources.

Linda Young

2011-02-23T23:59:59.000Z

129

The Growth of Supermassive Black Holes Across Cosmic Time  

E-Print Network (OSTI)

One of the main themes in extragalactic astronomy for the next decade will be the evolution of galaxies over cosmic time. Many future observatories, including JWST, ALMA, GMT, TMT and E-ELT will intensively observe starlight over a broad redshift range, out to the dawn of the modern Universe when the first galaxies formed. It has, however, become clear that the properties and evolution of galaxies are intimately linked to the growth of their central black holes. Understanding the formation of galaxies, and their subsequent evolution, will therefore be incomplete without similarly intensive observations of the accretion light from supermassive black holes (SMBH) in galactic nuclei. To make further progress, we need to chart the formation of typical SMBH at z>6, and their subsequent growth over cosmic time, which is most effectively achieved with X-ray observations. Recent technological developments in X-ray optics and instrumentation now bring this within our grasp, enabling capabilities fully matched to those...

Nandra, K; Alexander, D M; Ballantyne, D R; Barcons, X; Bauer, F E; Boller, T; Brandt, W N; Brusa, M; Cattaneo, A; Chartas, G; Coil, A L; Comastri, A; Croton, D J; Della Ceca, R; Dickinson, M; Fabian, A C; Fazio, G G; Fiore, F; Flanagan, K A; Forman, W R; Gehrels, N; Georgakakis, A; Georgantopoulos, I; Gilli, R; Hasinger, G; Hopkins, P F; Hornschemeier, A E; Ivison, R J; Kauffmann, G; King, A R; Koekemoer, A M; Koo, D C; Kunieda, H; Laird, E S; Levenson, N A; Li, Y; Madau, P; Ohashi, T; Pounds, K A; Primack, J R; Ranalli, P; Ricker, G R; Rossi, E M; Shemmer, O; Somerville, R S; Stern, D; Stiavelli, M; Tananbaum, H; Terashima, Y; Treister, E; Ueda, Y; Vignali, C; Volonteri, M; Watson, M G; White, N E; White, S D M

2009-01-01T23:59:59.000Z

130

Cosmic string induced CMB maps  

SciTech Connect

We compute maps of CMB temperature fluctuations seeded by cosmic strings using high resolution simulations of cosmic strings in a Friedmann-Robertson-Walker universe. We create full-sky, 18 deg. and 3 deg. CMB maps, including the relevant string contribution at each resolution from before recombination to today. We extract the angular power spectrum from these maps, demonstrating the importance of recombination effects. We briefly discuss the probability density function of the pixel temperatures, their skewness, and kurtosis.

Landriau, M. [Max-Planck-Institut fuer extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching (Germany); Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Centre for Mathematical Sciences, Wilberforce Road, Cambridge CB3 0WA (United Kingdom); Shellard, E. P. S. [Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Centre for Mathematical Sciences, Wilberforce Road, Cambridge CB3 0WA (United Kingdom)

2011-02-15T23:59:59.000Z

131

The Center for Frontiers of Subsurface Energy Security (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

SciTech Connect

'The Center for Frontiers of Subsurface Energy Security (CFSES)' was submitted to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. CFSES is directed by Gary A. Pope at the University of Texas at Austin and partners with Sandia National Laboratories. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges.

Pope, Gary A. (Director, Center for Frontiers of Subsurface Energy Security); CFSES Staff

2011-05-01T23:59:59.000Z

132

Energy Frontier Research Center Materials Science of Actinides (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

SciTech Connect

'Energy Frontier Research Center Materials Science of Actinides' was submitted by the EFRC for Materials Science of Actinides (MSA) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. MSA is directed by Peter Burns at the University of Notre Dame, and is a partnership of scientists from ten institutions.The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges.

Burns, Peter (Director, Materials Science of Actinides); MSA Staff

2011-05-01T23:59:59.000Z

133

Lithium-6 and Gamma Rays: Complementary Constraints on Cosmic-Ray History  

E-Print Network (OSTI)

The rare isotope 6Li is made only by cosmic rays, dominantly in alpha+alpha fusion reactions with ISM helium. Consequently, this nuclide provides a unique diagnostic of the history of cosmic rays in our Galaxy. The same hadronic cosmic-ray interactions also produce high-energy gamma rays (mostly via neutral pion production). Thus, hadronic gamma-rays and 6Li are intimately linked. Specifically, 6Li directly encodes the local cosmic-ray fluence over cosmic time, while extragalactic hadronic gamma rays encode an average cosmic-ray fluence over lines of sight out to the horizon. We examine this link and show how 6Li and gamma-rays can be used together to place important model-independent limits on the cosmic-ray history of our Galaxy and the universe. We first constrain gamma-ray production from ordinary Galactic cosmic rays, using the local 6Li abundance. We find that the solar 6Li abundance demands an accompanying extragalactic pionic gamma-ray intensity which exceeds that of the entire observed EGRB by a factor of 2-6. Possible explanations for this discrepancy are discussed. We then constrain Li production using recent determinations of extragalactic gamma-ray background (EGRB). We note that cosmic rays created during cosmic structure formation would lead to pre-Galactic Li production, which would act as a "contaminant" to the primordial 7Li content of metal-poor halo stars. We find the uncertainties in the observed EGRB are so large that we cannot exclude a pre-Galactic Li which is comparable to primordial 7Li. Our limits and their more model-dependent extensions will improve significantly with additional observations of 6Li in halo stars, and with improved measurements of the EGRB spectrum by GLAST. (Abriged abstract)

Brian D. Fields; Tijana Prodanovic

2004-07-15T23:59:59.000Z

134

Clusters and the Cosmic Web  

E-Print Network (OSTI)

We discuss the intimate relationship between the filamentary features and the rare dense compact cluster nodes in this network, via the large scale tidal field going along with them, following the cosmic web theory developed Bond et al. The Megaparsec scale tidal shear pattern is responsible for the contraction of matter into filaments, and its link with the cluster locations can be understood through the implied quadrupolar mass distribution in which the clusters are to be found at the sites of the overdense patches. We present a new technique for tracing the cosmic web, identifying planar walls, elongated filaments and cluster nodes in the galaxy distribution. This will allow the practical exploitation of the concept of the cosmic web towards identifying and tracing the locations of the gaseous WHIM. These methods, the Delaunay Tessellation Field Estimator (DTFE) and the Morphology Multiscale Filter (MMF) find their basis in computational geometry and visualization.

Rien van de Weygaert

2006-07-24T23:59:59.000Z

135

Expanding the Frontiers of Visual Analytics and Visualization  

Science Conference Proceedings (OSTI)

Expanding the Frontiers of Visual Analytics and Visualization contains international contributions by leading researchers from within the field. Dedicated to the memory of Jim Thomas, the book begins with the dynamics of evolving a vision based on some of the principles that Jim and colleagues established and in which Jim’s leadership was evident. This is followed by chapters in the areas of visual analytics, visualization, interaction, modelling, architecture, and virtual reality, before concluding with the key area of technology transfer to industry.

Dill, John; Earnshaw, Rae; Kasik, David; Vince, John; Wong, Pak C.

2012-05-31T23:59:59.000Z

136

Howdy pardner!: on free-to-play, sociability and rhythm design in FrontierVille  

Science Conference Proceedings (OSTI)

Despite their rapid evolution and wide popularity social games played on Facebook have so far gained relatively little interest among academic game researchers. A close reading of the Facebook game FrontierVille aims to provide some starting points ... Keywords: FrontierVille, facebook, free-to-play, rhythm design, sociability, social games, social network games, virality, zynga

Heikki Tyni; Olli Sotamaa; Saara Toivonen

2011-09-01T23:59:59.000Z

137

High-energy Cosmic Rays  

E-Print Network (OSTI)

After a brief review of galactic cosmic rays in the GeV to TeV energy range, we describe some current problems of interest for particles of very high energy. Particularly interesting are two features of the spectrum, the `knee' above $10^{15}$ eV and the `ankle' above $10^{18}$ eV. An important question is whether the highest energy particles are of extra-galactic origin and, if so, at what energy the transition occurs. A theme common to all energy ranges is use of nuclear abundances as a tool for understanding the origin of the cosmic radiation.

Thomas K. Gaisser; Todor Stanev

2005-10-11T23:59:59.000Z

138

Life at the Frontiers of Energy Research Video Contest | U.S. DOE Office of  

Office of Science (SC) Website

Life at the Frontiers of Energy Research Life at the Frontiers of Energy Research Video Contest Energy Frontier Research Centers (EFRCs) EFRCs Home Centers Research Science Highlights News & Events EFRC News EFRC Events DOE Announcements Publications Contact BES Home 04.22.11 Life at the Frontiers of Energy Research Video Contest Print Text Size: A A A Subscribe FeedbackShare Page April 22, 2011 :: The Office of Science announced the winners of the Energy Frontier Research Centers Video Contest External link and the start of the People's Choice Contest External link . The video with the most votes by 5:00 pm on May 24, 2011 will receive the People's Choice Award. Be sure to vote for your favorites. The winning videos will be shown during an awards ceremony at the EFRC Summit External link on May 25, 2011. View the

139

U.S. Department of Energy Announces Energy Frontier Research Centers Summit  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Energy Frontier Research Energy Frontier Research Centers Summit & Forum U.S. Department of Energy Announces Energy Frontier Research Centers Summit & Forum March 4, 2011 - 12:00am Addthis Washington, D.C. -The U.S. Department of Energy (DOE) today announced the first Science for Our Nation's Energy Future: Energy Frontier Research Centers Summit & Forum to be held on May 25-27, 2011, at the Renaissance Penn Quarter hotel in Washington D.C. The Summit will bring together scientists and energy policy leaders to explore the challenges and opportunities in applying America's extraordinary scientific and technical resources to critical energy needs and will highlight early successes of the DOE's Energy Frontier Research Centers and promote collaboration across the national energy enterprise.

140

On the Origin of Ultra High Energy Cosmic Rays II  

Science Conference Proceedings (OSTI)

We show that accretion disks around Active Galactic Nuclei (AGNs) could account for the enormous power in observed ultra high energy cosmic rays {approx}10{sup 20} eV (UHEs). In our model, cosmic rays are produced by quasi-steady acceleration of ions in magnetic structures previously proposed to explain jets around Active Galactic Nuclei with supermassive black holes. Steady acceleration requires that an AGN accretion disk act as a dynamo, which we show to follow from a modified Standard Model in which the magnetic torque of the dynamo replaces viscosity as the dominant mechanism accounting for angular momentum conservation during accretion. A black hole of mass M{sub BH} produces a steady dynamo voltage V {proportional_to} {radical}M{sub BH} giving V {approx} 10{sup 20} volts for M{sub BH} {approx} 10{sup 8} solar masses. The voltage V reappears as an inductive electric field at the advancing nose of a dynamo-driven jet, where plasma instability inherent in collisionless runaway acceleration allows ions to be steadily accelerated to energies {approx} V, finally ejected as cosmic rays. Transient events can produce much higher energies. The predicted disk radiation is similar to the Standard Model. Unique predictions concern the remarkable collimation of jets and emissions from the jet/radiolobe structure. Given MBH and the accretion rate, the model makes 7 predictions roughly consistent with data: (1) the jet length; (2) the jet radius; (3) the steady-state cosmic ray energy spectrum; (4) the maximum energy in this spectrum; (5) the UHE cosmic ray intensity on Earth; (6) electron synchrotron wavelengths; and (7) the power in synchrotron radiation. These qualitative successes motivate new computer simulations, experiments and data analysis to provide a quantitative verification of the model.

Fowler, T K; Colgate, S; Li, H; Bulmer, R H; Pino, J

2011-03-08T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
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to obtain the most current and comprehensive results.


141

Reheating and Cosmic String Production  

E-Print Network (OSTI)

We compute the string production rate at the end of inflation, using the string spectrum obtained in \\lss in a near-de Sitter space. Our result shows that highly excited strings are hardly produced, thus the simple slow-roll inflation alone does not offer a cosmic string production mechanism.

Chao-Jun Feng; Xian Gao; Miao Li; Wei Song; Yushu Song

2007-07-06T23:59:59.000Z

142

Cosmic-ray sum rules  

SciTech Connect

We introduce new sum rules allowing to determine universal properties of the unknown component of the cosmic rays; we show how they can be used to predict the positron fraction at energies not yet explored by current experiments, and to constrain specific models.

Frandsen, Mads T. [Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Road, Oxford OX1 3NP (United Kingdom); Masina, Isabella [Dip. di Fisica dell'Universita di Ferrara and INFN Sez. di Ferrara, Via Saragat 1, I-44100 Ferrara (Italy); CP3-Origins, University of Southern Denmark, Campusvej 55, DK-5230 Odense M (Denmark); Sannino, Francesco [CP3-Origins, University of Southern Denmark, Campusvej 55, DK-5230 Odense M (Denmark)

2011-06-15T23:59:59.000Z

143

Cosmic Rays and the Monogem Supernova Remnant  

E-Print Network (OSTI)

Recent findings indicate that the Monogem Ring supernova remnant (SNR) and the associated pulsar B0656+14 may be the 'Single Source' responsible for the knee in the cosmic ray (CR) energy spectrum at ~3 PeV. We estimate the contribution of this pulsar to CR in the PeV region. We conclude that although the pulsar can contribute to the formation of the knee, it cannot be the domimant source and a SNR is still needed. We also examine the possibility of the pulsar giving the peak of the extensive air shower (EAS) intensity observed from the region inside the Monogem Ring. If the experimental EAS results concerning a narrow source are confirmed, they can be important, since they give evidence: (i) for the acceleration of protons and heavier nuclei by the pulsar; (ii) for the existence of the confinement mechanism in SNR; (iii) that CR produced by the Monogem Ring SNR and associated pulsar B0656+14 were released recently giving rise to the formation of the knee and the observed narrow peak in the EAS intensity; (iv) for the Monogem Ring and the associated pulsar B0656+14 being identified as the Single Source proposed in our Single Source Model of the knee. A number of predictions of the examined scenario are made.

A. D. Erlykin; A. W. Wolfendale

2004-04-27T23:59:59.000Z

144

Electron Ion Collider: The Next QCD Frontier Understanding  

NLE Websites -- All DOE Office Websites (Extended Search)

Electron Electron Ion Collider: The Next QCD Frontier Understanding the glue that binds us all White Paper Writing Committee Elke C. Aschenauer Brookhaven National Laboratory William Brooks Universidad T´ ecnica Federico Santa Maria Abhay Deshpande 1 Stony Brook University Markus Diehl Deutsches Elektronen-Synchrotron DESY Haiyan Gao Duke University Roy Holt Argonne National Laboratory Tanja Horn The Catholic University of America Andrew Hutton Thomas Jefferson National Accelerator Facility Yuri Kovchegov The Ohio State University Krishna Kumar University of Massachusetts, Amherst Zein-Eddine Meziani 1 Temple University Alfred Mueller Columbia University Jianwei Qiu 1 Brookhaven National Laboratory Michael Ramsey-Musolf University of Wisconsin Thomas Roser Brookhaven National Laboratory 1 Co-Editor 1 Franck Sabati´ e Commissariat ` a l' ´ Energie Atomique-Saclay

145

Fermilab | Science at Fermilab | Experiments & Projects | Energy Frontier |  

NLE Websites -- All DOE Office Websites (Extended Search)

Physics Physics Energy Frontier Fermilab's Contribution to LHC Physics Physics Fermilab is involved in most aspects of the Compact Muon Solenoid experiment. The CMS detector is designed to detect objects physicists identify as fundamental: electrons, muons, tau leptons, photons, quark jets and missing energy due to weakly interacting particles such as neutrinos. Massive particles, such as the theorized Higgs boson, will decay into these fundamental particles, and the CMS detector will measure their properties. Fermilab functions as the host laboratory for U.S. efforts in the CMS experiment through its LHC Physics Center, Remote Operations Center and the largest CMS computing center outside of CERN. About 120 Fermilab scientists, postdocs, visiting students, engineers and technicians

146

Report of the Snowmass 2013 energy frontier QCD working group  

E-Print Network (OSTI)

This is the summary report of the energy frontier QCD working group prepared for Snowmass 2013. We review the status of tools, both theoretical and experimental, for understanding the strong interactions at colliders. We attempt to prioritize important directions that future developments should take. Most of the efforts of the QCD working group concentrate on proton-proton colliders, at 14 TeV as planned for the next run of the LHC, and for 33 and 100 TeV, possible energies of the colliders that will be necessary to carry on the physics program started at 14 TeV. We also examine QCD predictions and measurements at lepton-lepton and lepton-hadron colliders, and in particular their ability to improve our knowledge of strong coupling constant and parton distribution functions.

J. M. Campbell; K. Hatakeyama; J. Huston; F. Petriello; J. Andersen; L. Barze; H. Beauchemin; T. Becher; M. Begel; A. Blondel; G. Bodwin; R. Boughezal; S. Carrazza; M. Chiesa; G. Dissertori; S. Dittmaier; G. Ferrera; S. Forte; N. Glover; T. Hapola; A. Huss; X. Garcia i Tormo; M. Grazzini; S. Hoche; P. Janot; T. Kasprzik; M. Klein; U. Klein; D. Kosower; Y. Li; X. Liu; P. Mackenzie; D. Maitre; E. Meoni; K. Mishra; G. Montagna; M. Moretti; P. Nadolsky; O. Nicrosini; F. Piccinini; L. Reina; V. Radescu; J. Rojo; J. Russ; S. Sapeta; A. Schwartzman; P. Skands; J. Smillie; I. W. Stewart; F. J. Tackmann; F. Tramontano; R. Van de Water; J. R. Walsh; S. Zuberi

2013-10-19T23:59:59.000Z

147

Masatoshi Koshiba and Cosmic Neutrinos  

Office of Scientific and Technical Information (OSTI)

Masatoshi Koshiba and Cosmic Neutrinos Masatoshi Koshiba and Cosmic Neutrinos Resources with Additional Information Masatoshi Koshiba Courtesy of Sebastian Brandt 'The 2002 Nobel Prize in Physics has been awarded to ... Masatoshi Koshiba of the International Center for Elementary Particle Physics at the University of Tokyo in Japan, ... "for pioneering contributions to astrophysics, in particular for the detection of cosmic neutrinos." ... Neutrinos are important in astrophysics since they might have played a considerable role in shaping early galaxies; they are the form of energy coming directly from the solar core; and they account for the largest share of energy released during supernova explosions....'1 ...Koshiba, professor emeritus at the University of Tokyo, received his doctorate from the University of Rochester in [1955]. This year [2000], he is the co-recipient of the Wolf Prize in Physics, considered second only to the Nobel Prize in prestige, for his discovery that neutrinos have mass. Neutrinos are tiny particles smaller than atoms, and Koshiba's discovery is being hailed for its ramifications in the study of astronomical objects and the fundamental properties of matter, helping scientists to understand the birth of the universe. Koshiba started his career as a research associate at the University of Rochester, then went on to teach at the University of Tokyo." 2

148

Secretary Bodman Praises Western States' "Frontier Line" | Department of  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Praises Western States' "Frontier Line" Praises Western States' "Frontier Line" Secretary Bodman Praises Western States' "Frontier Line" April 5, 2005 - 11:30am Addthis WASHINGTON, DC - Secretary of Energy Samuel W. Bodman today released the following statement regarding the "Frontier Line" announced by Governors Arnold Schwarzenegger (CA), Kenny Guinn (NV), Jon Huntsman (UT), and David Freudenthal (WY): "This proposal exhibits the boldness and innovation the West is traditionally known for, as well as the multi-state cooperation and big-picture thinking required to make regional markets thrive," Secretary Bodman said. "At the federal level, the President's comprehensive energy strategy that Congress will begin working on this week calls for upgrades to our electric grid to help prevent future brownouts or

149

Los Alamos engineer selected to participate in NAE's 2012 "Frontiers of  

NLE Websites -- All DOE Office Websites (Extended Search)

Moody to participate in "Frontiers of Engineering" Moody to participate in "Frontiers of Engineering" Los Alamos engineer selected to participate in NAE's 2012 "Frontiers of Engineering" symposium Engineers between 30 to 45 who are performing exceptional engineering research and technical work in a variety of disciplines attend the 2-1/2 day event. August 22, 2012 Nathan Moody Nathan Moody Contact Nancy Ambrosiano Communications Office (505) 667-0471 Email Nathan Moody, specialist in electromagnetic radiation, honored LOS ALAMOS, NEW MEXICO, August 22, 2012-Nathan Moody of Los Alamos National Laboratory is among 78 of the nation's brightest young engineers selected for the National Academy of Engineering's (NAE) 18th annual U.S. Frontiers of Engineering symposium. Engineers between 30 to 45 who are

150

Energy Frontier Research Centers (EFRCs) Homepage | U.S. DOE Office of  

Office of Science (SC) Website

EFRCs Home EFRCs Home Energy Frontier Research Centers (EFRCs) EFRCs Home Centers Research Science Highlights News & Events Publications Contact BES Home Print Text Size: A A A RSS Feeds FeedbackShare Page Energy Frontier Research Centers As world demand for energy rapidly expands, transforming the way we generate, supply, transmit, store, and use energy will be one of the defining challenges for America and the globe in the 21st century. At its heart, the challenge is a scientific one. Important as they are, incremental advances in current energy technologies will not be sufficient. History has demonstrated that radically new technologies arise from disruptive advances at the science frontiers. The Energy Frontier Research Centers program aims to accelerate such transformative discovery, combining

151

DOE Awards $377 Million in Funding for 46 Energy Frontier Research Centers  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

DOE Awards $377 Million in Funding for 46 Energy Frontier Research DOE Awards $377 Million in Funding for 46 Energy Frontier Research Centers DOE Awards $377 Million in Funding for 46 Energy Frontier Research Centers August 6, 2009 - 12:00am Addthis Washington, DC - In a major effort to accelerate the scientific breakthroughs needed to build a new 21st-century energy economy, U.S. Energy Secretary Steven Chu announced the delivery of $377 million in funding for 46 new multi-million-dollar Energy Frontier Research Centers (EFRCs) located at universities, national laboratories, nonprofit organizations, and private firms across the nation. "As global energy demand grows, there is an urgent need to reduce our dependence on imported oil and curtail greenhouse gas emissions," said Secretary Chu. "Meeting the challenge to reduce our dependence on

152

Search for Topological Phases New Frontiers in Low-Dimensional Systems Program  

E-Print Network (OSTI)

Search for Topological Phases of Matter New Frontiers in Low-Dimensional Systems Program 21 will be to identify the most promising future directions in the search for topological phases, as well as to formulate

153

Frontiers in Assessing the Role of Chemical Speciation and Natural Attenuation on the Bioavailability  

E-Print Network (OSTI)

1 Frontiers in Assessing the Role of Chemical Speciation and Natural Attenuation of contaminants in the terrestrial environment is greatly affected by a number of chemical factors and processes its fate, transport, and bioavailability. Traditionally, chemical extraction techniques have been

Sparks, Donald L.

154

Life at the Frontiers of Energy Research Video Contest | U.S...  

Office of Science (SC) Website

1 Life at the Frontiers of Energy Research Video Contest News In the News In Focus 2013 2012 2011 2010 2009 2008 2007 2006 2005 Presentations & Testimony Recovery Act Contact...

155

Frontier market analysis : a case study of Iraq's real estate industry  

E-Print Network (OSTI)

Success in frontier markets could mean high returns for real estate developers and investors. In order to succeed, companies must determine how to provide their products or services in an environment that may not necessarily ...

Watkins, Steven C., Jr. (Steven Charles)

2010-01-01T23:59:59.000Z

156

DOE Awards $377 Million in Funding for 46 Energy Frontier Research Centers  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

77 Million in Funding for 46 Energy Frontier Research 77 Million in Funding for 46 Energy Frontier Research Centers DOE Awards $377 Million in Funding for 46 Energy Frontier Research Centers August 6, 2009 - 12:00am Addthis Washington, DC - In a major effort to accelerate the scientific breakthroughs needed to build a new 21st-century energy economy, U.S. Energy Secretary Steven Chu announced the delivery of $377 million in funding for 46 new multi-million-dollar Energy Frontier Research Centers (EFRCs) located at universities, national laboratories, nonprofit organizations, and private firms across the nation. "As global energy demand grows, there is an urgent need to reduce our dependence on imported oil and curtail greenhouse gas emissions," said Secretary Chu. "Meeting the challenge to reduce our dependence on

157

Electricity: The Energy of Tomorrow (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'Electricity: the Energy of Tomorrow' was submitted by the Energy Materials Center at Cornell (emc2) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. emc2, an EFRC directed by Hector D. Abruna at Cornell University (lead) is a partnership between Cornell and Lawrence Berkeley National Laboratory. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges.

Abruna, Hector D. (Director, Energy Materials Center at Cornell); emc2 Staff

2011-05-01T23:59:59.000Z

158

PARC - Scientific Exchange Program (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'PARC - Scientific Exchange Program' was submitted by the Photosynthetic Antenna Research Center (PARC) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. PARC, an EFRC directed by Robert E. Blankenship at Washington University in St. Louis, is a partnership of scientists from ten institutions. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges.

Blankenship, Robert E. (Director, Photosynthetic Antenna Research Center); PARC Staff

2011-05-01T23:59:59.000Z

159

High-energy cosmic ray interactions  

SciTech Connect

Research into hadronic interactions and high-energy cosmic rays are closely related. On one hand--due to the indirect observation of cosmic rays through air showers--the understanding of hadronic multiparticle production is needed for deriving the flux and composition of cosmic rays at high energy. On the other hand the highest energy particles from the universe allow us to study the characteristics of hadronic interactions at energies far beyond the reach of terrestrial accelerators. This is the summary of three introductory lectures on our current understanding of hadronic interactions of cosmic rays.

Engel, Ralph [Forschungszentrum Karlsruhe, P.O. Box 3640, 76021 Karlsruhe (Germany); Orellana, Mariana [Instituto Argentino de Radioastronomia (IAR), CCT La Plata (CONICET), C.C.5, 1894 Villa Elisa, Buenos Aires (Argentina); Facultad de Ciencias Astronomicas y Geofisicas, Universidad Nacional de La Plata, Paseo del Bosque, 1900 La Plata (Argentina); Reynoso, Matias M. [Departamento de Fisica, Facultad de Ciencias Exactas y Naturales, Universidad Nacional de Mar del Plata, Funes 3350, (7600) Mar del Plata (Argentina); Instituto de Investigaciones Fisicas de Mar del Plata, (UNMdP-CONICET) (Argentina); Vila, Gabriela S. [Instituto Argentino de Radioastronomia (IAR), CCT La Plata (CONICET), C.C.5, 1894 Villa Elisa, Buenos Aires (Argentina)

2009-04-30T23:59:59.000Z

160

Center for Defect Physics - Energy Frontier Research Center (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

SciTech Connect

'Center for Defect Physics - Energy Frontier Research Center' was submitted by the Center for Defect Physics (CDP) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. CDP is directed by G. Malcolm Stocks at Oak Ridge National Laboratory, and is a partnership of scientists from nine institutions: Oak Ridge National Laboratory (lead); Ames Laboratory; Brown University; University of California, Berkeley; Carnegie Mellon University; University of Illinois, Urbana-Champaign; Lawrence Livermore National Laboratory; Ohio State University; and University of Tennessee. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges.

Stocks, G. Malcolm (Director, Center for Defect Physics in Structural Materials); CDP Staff

2011-05-01T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


161

EFRC:CST at the University of Texas at Austin - A DOE Energy Frontier Research Center (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'EFRC:CST at the University of Texas at Austin - A DOE Energy Frontier Research Center' was submitted by the EFRC for Understanding Charge Separation and Transfer at Interfaces in Energy Materials (EFRC:CST) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. EFRC:CST is directed by Xiaoyang Zhu at the University of Texas at Austin in partnership with Sandia National Laboratories. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges.

Zhu, Xiaoyang (Director, Understanding Charge Separation and Transfer at Interfaces in Energy Materials); CST Staff

2011-05-01T23:59:59.000Z

162

Transverse beam shape measurements of intense proton beams using optical transition radiation  

SciTech Connect

A number of particle physics experiments are being proposed as part of the Department of Energy HEP Intensity Frontier. Many of these experiments will utilize megawatt level proton beams onto targets to form secondary beams of muons, kaons and neutrinos. These experiments require transverse size measurements of the incident proton beam onto target for each beam spill. Because of the high power levels, most beam intercepting profiling techniques will not work at full beam intensity. The possibility of utilizing optical transition radiation (OTR) for high intensity proton beam profiling is discussed. In addition, previous measurements of OTR beam profiles from the NuMI beamline are presented.

Scarpine, Victor E.; /Fermilab

2012-03-01T23:59:59.000Z

163

NERSC Continues Tradition of Cosmic Microwave Background Data...  

NLE Websites -- All DOE Office Websites (Extended Search)

Tradition of Cosmic Microwave Background Data Analysis with the Planck Cluster NERSC Continues Tradition of Cosmic Microwave Background Data Analysis with the Planck...

164

Reading the Cosmic Writing on the Wall  

NLE Websites -- All DOE Office Websites (Extended Search)

Reading the Cosmic Reading the Cosmic Writing on the Wall Reading the Cosmic Writing on the Wall NERSC Key to Planck's Revision of Universal Recipe March 21, 2013 Contact: Margie Wylie, mwylie@lbl.gov, + 1 510 486 7421 map800-600.jpg This map shows the oldest light in our universe, as detected with the greatest precision yet by the Planck mission. The ancient light, called the cosmic microwave background, was imprinted on the sky when the universe was 370,000 years old. (Image credit: ESA and the Planck Collaboration) Thanks to a supersensitive space telescope and some sophisticated supercomputing, scientists from the international Planck collaboration have made the closest reading yet of the most ancient story in our universe: the cosmic microwave background (CMB). Today, the team released preliminary results based on the Planck

165

Extremely High Energy Neutrinos, Neutrino Hot Dark Matter, and the Highest Energy Cosmic Rays  

E-Print Network (OSTI)

Extremely high energy (up to 10**(22) eV) cosmic neutrino beams initiate high energy particle cascades in the background of relic neutrinos from the Big Bang. We perform numerical calculations to show that such cascades could contribute more than 10% to the observed cosmic ray flux above 10**(19) eV if neutrinos have masses in the electron volt range. The required intensity of primary neutrinos could be consistent with astrophysical models for their production if the maximum neutrino energy reaches to 10**(22) eV and the massive neutrino dark matter is locally clustered. Future observations of ultra high energy cosmic rays will lead to an indirect but practical search for neutrino dark matter.

Shigeru Yoshida; Guenter Sigl; Sangjin Lee

1998-08-14T23:59:59.000Z

166

Cosmic Growth History and Expansion History  

E-Print Network (OSTI)

The cosmic expansion history tests the dynamics of the global evolution of the universe and its energy density contents, while the cosmic growth history tests the evolution of the inhomogeneous part of the energy density. Precision comparison of the two histories can distinguish the nature of the physics responsible for the accelerating cosmic expansion: an additional smooth component - dark energy - or a modification of the gravitational field equations. With the aid of a new fitting formula for linear perturbation growth accurate to 0.05-0.2%, we separate out the growth dependence on the expansion history and introduce a new growth index parameter \\gamma that quantifies the gravitational modification.

Eric V. Linder

2005-07-11T23:59:59.000Z

167

TransForum v9n2 - Energy Frontier Research Centers  

NLE Websites -- All DOE Office Websites (Extended Search)

Energy Frontier Research Centers Promise Advances in Transportation Technologies Energy Frontier Research Centers Promise Advances in Transportation Technologies IACT The solid-electrolyte interface is a critical component in electrochemical energy storage. Because of the high reactivity between the electrolyte and the electrodes at the SEI interface, Li-ion batteries show limited calendar and cycle life--less than two years, which is much lower than the 15 years required for enabling this technology in vehicles. CEES The platinum particle is interacting with a molecule of propanol. The propanol is a gas phase surrogate for the heavier cellulose materials that are the focus of one of Argonne's Energy Frontier Research Centers, the Institute for Atom-Efficient Chemical Transformations. The U.S. Department of Energy's (DOE's) Office of Science recently

168

On the Frontiers of a New Energy Source | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

On the Frontiers of a New Energy Source On the Frontiers of a New Energy Source On the Frontiers of a New Energy Source May 2, 2012 - 3:59pm Addthis Building on this initial, small-scale test, the Department is launching a new research effort to conduct a long-term production test in the Arctic. Building on this initial, small-scale test, the Department is launching a new research effort to conduct a long-term production test in the Arctic. Secretary Chu Secretary Chu Former Secretary of Energy What are the key facts? Methane hydrates are 3D ice-lattice structures with natural gas locked inside. The United States has an abundance of this untapped resource - methane hydrates are found in and under the Arctic permafrost and in ocean sediments along nearly every continental shelf in the world. Today, we're announcing that the Department of Energy, along with the

169

On the Frontiers of a New Energy Source | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

On the Frontiers of a New Energy Source On the Frontiers of a New Energy Source On the Frontiers of a New Energy Source May 2, 2012 - 3:59pm Addthis Building on this initial, small-scale test, the Department is launching a new research effort to conduct a long-term production test in the Arctic. Building on this initial, small-scale test, the Department is launching a new research effort to conduct a long-term production test in the Arctic. Secretary Chu Secretary Chu Former Secretary of Energy What are the key facts? Methane hydrates are 3D ice-lattice structures with natural gas locked inside. The United States has an abundance of this untapped resource - methane hydrates are found in and under the Arctic permafrost and in ocean sediments along nearly every continental shelf in the world. Today, we're announcing that the Department of Energy, along with the

170

Approaches to renewable energy storage focus of Frontiers in Science talk  

NLE Websites -- All DOE Office Websites (Extended Search)

Frontiers in Science Talk Frontiers in Science Talk Approaches to renewable energy storage focus of Frontiers in Science talk Albert Migliori will give the series of public talks, titled, "Use It, Lose It, or Save It: The Science of Renewable Energy Storage." August 21, 2008 Los Alamos National Laboratory sits on top of a once-remote mesa in northern New Mexico with the Jemez mountains as a backdrop to research and innovation covering multi-disciplines from bioscience, sustainable energy sources, to plasma physics and new materials. Los Alamos National Laboratory sits on top of a once-remote mesa in northern New Mexico with the Jemez mountains as a backdrop to research and innovation covering multi-disciplines from bioscience, sustainable energy sources, to plasma physics and new materials.

171

Measuring the relative efficiency of IC design firms using the directional distance function and a meta-frontier approach  

Science Conference Proceedings (OSTI)

This paper presents an alternative approach for evaluating the efficiency of integrated circuit (IC) design firms. In doing so, it accounts for differences between technology groups containing one or more design firms, and input and output factors to ... Keywords: Directional distance function, Group-frontier, IC design firm, Meta-frontier, Performance evaluations

Bo Hsiao; Ching-Chin Chern; Ming-Miin Yu

2012-11-01T23:59:59.000Z

172

Are High Energy Cosmic Rays Magnetic Monopoles?  

E-Print Network (OSTI)

We argue that magnetic monopoles can not be associated to the highest energy cosmic rays as recently suggested. Both the observed spectrum and the arrival direction disagree with observation.

C. O. Escobar; R. A. Vázquez

1997-09-15T23:59:59.000Z

173

Cosmic ray propagation in galactic turbulence  

E-Print Network (OSTI)

We revisit propagation of galactic cosmic rays in light of recent advances in cosmic ray diffusion theory in realistic interstellar turbulence. We use tested model of turbulence in which it has been shown that fast modes dominate scattering of cosmic rays. As a result, propagation becomes inhomogeneous and environment dependent. By adopting the formalism of the nonlinear theory (NLT) developed by Yan & Lazarian (2008), we calculate diffusion of cosmic rays self-consistently from first principles. We assume a two-phase model for the Galaxy to account for different damping mechanisms of the fast modes, and we find that the energy dependence of the diffusion coefficient is mainly affected by medium properties. We show that it gives a correct framework to interpret some of the recent CR puzzles.

Evoli, Carmelo

2013-01-01T23:59:59.000Z

174

Gamma Ray Bursts from Ordinary Cosmic Strings  

E-Print Network (OSTI)

We give an upper estimate for the number of gamma ray bursts from ordinary (non-superconducting) cosmic strings expected to be observed at terrestrial detectors. Assuming that cusp annihilation is the mechanism responsible for the bursts we consider strings arising at a GUT phase transition and compare our estimate with the recent BATSE results. Further we give a lower limit for the effective area of future detectors designed to detect the cosmic string induced flux of gamma ray bursts.

R. H. Brandenberger; A. T. Sornborger; M. Trodden

1993-02-12T23:59:59.000Z

175

Radiodetection of Cosmic Ray Extensive Air Showers  

E-Print Network (OSTI)

We present the characteristics and performance of a demonstration experiment devoted to the observation of ultra high- energy cosmic ray extensive air showers using a radiodetection technique. In a first step, one antenna narrowed band filtered acting as trigger, with a 4 $\\sigma$ threshold above sky background-level, was used to tag any radio transient in coincidence on the antenna array. Recently, the addition of 4 particle detectors has allowed us to observe cosmic ray events in coincidence with antennas.

D. Ardouin; A. Belletoile; D. Charrier; R. Dallier; L. Denis; P. Eschstruth; T. Gousset; F. Haddad; J. Lamblin; P. Lautridou; A. Lecacheux; D. Monnier-Ragaiggne; A. Rahmani; O. Ravel; the Codalema Collaboration

2004-12-09T23:59:59.000Z

176

ENERGY SPECTRA OF COSMIC-RAY NUCLEI AT HIGH ENERGIES  

SciTech Connect

We present new measurements of the energy spectra of cosmic-ray (CR) nuclei from the second flight of the balloon-borne experiment Cosmic-Ray Energetics And Mass (CREAM). The instrument included different particle detectors to provide redundant charge identification and measure the energy of CRs up to several hundred TeV. The measured individual energy spectra of C, O, Ne, Mg, Si, and Fe are presented up to approx10{sup 14} eV. The spectral shape looks nearly the same for these primary elements and it can be fitted to an E {sup -2.66} {sup +}- {sup 0.04} power law in energy. Moreover, a new measurement of the absolute intensity of nitrogen in the 100-800 GeV/n energy range with smaller errors than previous observations, clearly indicates a hardening of the spectrum at high energy. The relative abundance of N/O at the top of the atmosphere is measured to be 0.080 +- 0.025 (stat.)+-0.025 (sys.) at approx800 GeV/n, in good agreement with a recent result from the first CREAM flight.

Ahn, H. S.; Ganel, O.; Han, J. H.; Kim, K. C.; Lee, M. H.; Malinine, A. [Institute for Physical Science and Technology, University of Maryland, College Park, MD 20742 (United States); Allison, P.; Beatty, J. J.; Brandt, T. J. [Department of Physics, Ohio State University, Columbus, OH 43210 (United States); Bagliesi, M. G.; Bigongiari, G.; Maestro, P.; Marrocchesi, P. S. [Department of Physics, University of Siena and INFN, Via Roma 56, 53100 Siena (Italy); Barbier, L. [Astroparticle Physics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Childers, J. T.; DuVernois, M. A. [School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455 (United States); Conklin, N. B.; Coutu, S. [Department of Physics, Penn State University, University Park, PA 16802 (United States); Jeon, J. A. [Department of Physics, Ewha Womans University, Seoul 120-750 (Korea, Republic of); Minnick, S., E-mail: paolo.maestro@pi.infn.i [Department of Physics, Kent State University, Tuscarawas, New Philadelphia, OH 44663 (United States)

2009-12-10T23:59:59.000Z

177

CABS: Green Energy for Our Nation's Future (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'CABS: Green Energy for our Nation's Future' was submitted by the Center for Advanced Biofuel Systems (CABS) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. CABS, an EFRC directed by Jan Jaworski at the Donald Danforth Plant Science Center is a partnership of scientists from five institutions: Donald Danforth Plant Science Center (lead), Michigan State University, the University of Nebraska, New Mexico Consortium/LANL, and Washington State University. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges.

Jan Jaworski (Director, Center for Advanced Biofuel Systems); Sayre, Richard T. (previous Director); CABS Staff

2011-05-01T23:59:59.000Z

178

Inverse Design: Playing "Jeopardy" in Materials Science (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'Inverse Design: Playing 'Jeopardy' in Materials Science' was submitted by the Center for Inverse Design (CID) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. CID, an EFRC directed by Bill Tumas at the National Renewable Energy Laboratory is a partnership of scientists from five institutions: NREL (lead), Northwestern University, University of Colorado, Stanford University, and Oregon State University. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of the Center for Inverse Design is 'to replace trial-and-error methods used in the development of materials for solar energy conversion with an inverse design approach powered by theory and computation.' Research topics are: solar photovoltaic, photonic, metamaterial, defects, spin dynamics, matter by design, novel materials synthesis, and defect tolerant materials.

Alex Zunger (former Director, Center for Inverse Design); Tumas, Bill (Director, Center for Inverse Design); CID Staff

2011-05-01T23:59:59.000Z

179

Battle against Phonons (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum  

DOE Green Energy (OSTI)

'Battle against Phonons' was submitted by the Solid-State Solar-Thermal Energy Conversion (S3TEC) EFRC to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. This video was selected as one of five winners by a distinguished panel of judges for the special award, 'Best with Popcorn'. S3TEC, an EFRC directed by Gang Chen at the Massachusetts Institute of Technology is a partnership of scientists from four research institutions: MIT (lead), Oak Ridge National Laboratory, Boston College, and Rensselaer Polytechnic Institute. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of the Solid-State Solar Thermal Energy Conversion Center is 'to create novel, solid-state materials for the conversion of sunlight into electricity using thermal and photovoltaic processes.' Research topics are: solar photovoltaic, photonic, metamaterial, optics, solar thermal, thermoelectric, phonons, thermal conductivity, defects, ultrafast physics, interfacial characterization, matter by design, novel materials synthesis, charge transport, defect tolerant materials, and scalable processing.

Chen, Gang (Director, Solid-State Solar-Thermal Energy Conversion Center); S3TEC Staff

2011-05-01T23:59:59.000Z

180

UNC EFRC: Fuels from Sunlight (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'Fuels from Sunlight' was submitted by the University of North Carolina (UNC) EFRC: Solar Fuels and Next Generation Photovoltaics to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. The UNC EFRC directed by Thomas J. Meyer is a partnership of scientists from six institutions: UNC (lead), Duke University, University of Florida, North Caroline Central University, North Carolina State University, and the Research Triangle Institute. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of Solar Fuels and Next Generation Photovoltaics is 'to combine the best features of academic and translational research to study light/matter interactions and chemical processes for the efficient collection, transfer, and conversion of solar energy into chemical fuels and electricity.' Research topics are: catalysis (CO{sub 2}, hydrocarbons, water), electrocatalysis, photocatalysis, photoelectrocatalysis, solar photovoltaic, solar fuels, photonic, solar electrodes, photosynthesis, fuel cells, CO{sub 2} (convert), greenhosue gas, hydrogen (fuel), interfacial characterization, novel materials synthesis, charge transport, and self-assembly.

Meyer, Thomas J. (Director, UNC EFRC: Solar Fuels and Next Generation Photovoltaics); UNC EFRC Staff

2011-05-01T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


181

Enabling Energy Efficiency (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'Enabling Energy Efficiency' was submitted by the EFRC for Solid-State Lighting Science (SSLS) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. SSLS is directed by Mike Coltrin (Acting) and Jerry Simmons at Sandia National Laboratories, and is a partnership of scientists from eight institutions: Sandia National Laboratories (lead); California Institute of Technology; Los Alamos National Laboratory; University of Massachusetts, Lowell; University of New Mexico; Northwestern University; Philips Lumileds Lighting; and Rensselaer Polytechnic Institute. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges.

Coltrin, Mike (Acting Director, EFRC for Solid State Lighting Science); Simmons, Jerry; SSLS Staff

2011-05-01T23:59:59.000Z

182

Liquid Sunshine to Fuel Your Car (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'Liquid Sunshine to Fuel Your Car' was submitted by the Center for Lignocellulose Structure and Formation (CLSF) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. CLSF is directed by Daniel Cosgrove at Pennsylvania State University and is a partnership of scientists from three institutions: Penn State (lead), North Caroline State University, and Virginia Tech University. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of the Center for Lignocellulose Structure and Formation is 'to dramatically increase our fundamental knowledge of the formation and physical interactions of bio-polymer networks in plant cell walls to provide a basis for improved methods for converting biomass into fuels.' Research topics are: biofuels (biomass), membrane, interfacial characterization, matter by design, and self-assembly.

Cosgrove, Daniel (Director, Center for Lignocellulose Structure and Formation); CLSF Staff

2011-05-01T23:59:59.000Z

183

Saving the Sun for a Rainy Day (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'Saving the Sun for a Rainy Day' was submitted by the Center for Molecular Electrocatalysis (CME) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. CME, an EFRC directed by R. Morris Bullock at Pacific Northwest National Laboratory is a partnership of scientists from four institutions: PNNL (lead), Pensylvania State University, University of Washington, and the University of Wyoming. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of the Center for Molecular Electrocatalysis is 'to understand, design and develop molecular electrocatalysts for solar fuel production and use.' Research topics are: catalysis (water), electrocatalysis, bio-inspired, electrical energy storage, fuel cells, hydrogen (fuel), matter by design, novel materials synthesis, and charge transport.

Bullock, R. Morris (Director, Center for Molecular Electrocatalysis); CME Staff

2011-05-01T23:59:59.000Z

184

Excited About Excitons (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'Excited about Excitons' was submitted by the Center for Excitonics to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. This video was selected as one of five winners by a distinguished panel of judges for its 'outstanding portrayal of young scientists'. The Center for Excitonics, an EFRC directed by Marc Baldo at the Massachusetts Institute of Technology (MIT) is a partnership of scientists from three institutions: MIT (lead), Brookhaven National Laboratory, and Harvard University. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of the Center for Excitonics is 'to understand the transport of charge carriers in synthetic disordered systems, which hold promise as new materials for conversion of solar energy to electricity and electrical energy storage.' Research topics are: solar photovoltaic, photonic, solid state lighting, photosynthesis, novel materials synthesis, charge transport, defect tolerant materials, scalable processing, and self-assembly.

Baldo, Marc (Director, Center for Excitonics); Center for Excitonics Staff

2011-05-01T23:59:59.000Z

185

Search for the ANSER (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum  

DOE Green Energy (OSTI)

'Search for the ANSER' was submitted by the Argonne-Northwestern Solar Energy Research Center (ANSER) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. ANSER, an EFRC directed by Michael Wasielewski at Argonne National Laboratory is a partnership of scientists from five institutions: Argonne National Laboratory, Northwestern University, University of Chicago, University of Illinois at Urbana-Champaign, and Yale. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. At ANSER, the mission is 'to revolutionize our understanding of molecules, materials and methods necessary to create dramatically more efficient technologies for solar fuels and electricity production.' Research topics are: catalysis (water), electrocatalysis, photocatalysis, photoelectrocatalysis, solar photovoltaic, solar fuels, solar electrodes, photosynthesis, transportation fuels, bio-inspired, spin dynamics, hydrogen (fuel), ultrafast physics, interfacial characterization, matter by design, novel materials synthesis, charge transport, and self-assembly.

Wasielewski, Michael R. (Director, Argonne-Northwestern Solar Energy Research Center); ANSER Staff

2011-05-01T23:59:59.000Z

186

Gravity's Cosmic ShadowsGravity's Cosmic Shadows A Mathematical UnveilingA Mathematical Unveiling  

E-Print Network (OSTI)

Gravity's Cosmic ShadowsGravity's Cosmic Shadows A Mathematical UnveilingA Mathematical Unveiling of gravity on light SUNSUN #12;Gravitational Lensing - action of gravity on light SUNSUN #12;Gravitational Lensing - action of gravity on light SUNSUN nn 1801: Johann von1801: Johann von SoldnerSoldner (Newtonian

Weinberger, Hans

187

Distant Supernovae and Cosmic Deceleration  

E-Print Network (OSTI)

Distant supernovae can now be detected routinely. To date 34 supernovae at $z > 0.1$ have been discovered. Among them are 12 Type~Ia supernovae confirmed spectroscopically and suited to measure the cosmic deceleration when appropriately employed as standard candles. However, peak magnitudes have been determined for only two objects so far and a determination of $q_0$ is not yet possible. We describe the current status of the searches and possible pitfalls of the method which rests on few basic assumptions. The importance of sufficient information on the distant events is stressed and the observations of SN~1995K are used as an example of the detailed procedures employed in the analysis. Only spectroscopic classification and light curves in at least two filter bands provide the basis to use correction schemes for the luminosity which have successfully been established in nearby samples. Time dilation has been detected acting on the light curve of SN~1995K at a redshift of 0.478, providing clear evidence of universal expansion. The observations are fully consistent with local Type Ia supernovae in an expanding universe but incompatible with the expectations from a static universe. The contributions of the new, large telescopes to this research area are described. The extension of the observations to even more distant objects will provide a better leverage to distinguish between the possible decelerations and the inclusion of Type II supernovae into the sample add an independent check on the cosmological distances.

B. Leibundgut; J. Spyromilio

1996-08-22T23:59:59.000Z

188

Frontiers: Research highlights 1946-1996 [50th Anniversary Edition. Argonne National Laboratory  

SciTech Connect

This special edition of 'Frontiers' commemorates Argonne National Laboratory's 50th anniversary of service to science and society. America's first national laboratory, Argonne has been in the forefront of U.S. scientific and technological research from its beginning. Past accomplishments, current research, and future plans are highlighted.

NONE

1996-12-31T23:59:59.000Z

189

Managing uncertainty and ambiguity in frontier R&D projects: A Korean case study  

Science Conference Proceedings (OSTI)

One of the important tasks in planning large, frontier R&D projects is to minimize innate uncertainties and ambiguities in the early stages of the project. This case study is an attempt to provide a framework to handle such problems in R&D planning. ... Keywords: Fuzzy front-end, Knowledge management, O32, R&D planning, Technology management

Yong-Il Song; Dae-Hee Lee; Yong-Gil Lee; Yun-Chul Chung

2007-09-01T23:59:59.000Z

190

National Research Council Study on Frontiers in High-Energy-Density Physics  

E-Print Network (OSTI)

of Fusion Fusion Power Associates Washington, DC 19­21 November 2003 #12;E12541 High-energy-density physicsNational Research Council Study on Frontiers in High-Energy-Density Physics David D. Meyerhofer (HEDP) is a rapidly growing research area · Pressures in excess of 1 Mbar constitute high-energy

191

7016 EXPAnDing tHE fROntiERS Solar Decathlon team, circa 2005  

E-Print Network (OSTI)

7016 ­ EXPAnDing tHE fROntiERS #12;Solar Decathlon team, circa 2005 #12;CONCRETE CANOE;Above: ASCE (Class of Spring 1978) - Reunion, circa October 2007 Photo credit: Ralph Wheeler and Bob, then with the written part of the requirement, this added burden represented at least one additional credit hour

Aydilek, Ahmet

192

Edge Computing Edge Computing is pushing the frontier of computing applications, data, and services  

E-Print Network (OSTI)

Edge Computing Edge Computing is pushing the frontier of computing applications, data, and services not be continuously connected to a network such as laptops, smartphones, tablets and sensors. Edge Computing covers Cloud/Fog Computing and Grid/Mesh Computing, distributed data storage and retrieval, autonomic self

193

Production Economics Modeling and Analysis of Polluting firms: The Production Frontier Approach  

E-Print Network (OSTI)

As concern grows about energy and environment issues, energy and environmental modeling and related policy analysis are critical issues for today's society. Polluting firms such as coal power plants play an important role in providing electricity to drive the U.S. economy as well as producing pollution that damages the environment and human health. This dissertation is intended to model and estimate polluting firms' production using nonparametric methods. First, frontier production function of polluting firms is characterized by weak disposability between outputs and pollutants to reflecting the opportunity cost to reduce pollutants. The StoNED method is extended to estimate a weak disposability frontier production function accounting for random noise in the data. The method is applied to the U.S. coal power plants under the Acid Rain Program to find the average technical inefficiency and shadow price of SO2 and NOx. Second, polluting firms' production processes are modeled characterizing both the output production process and the pollution abatement process. Using the law of conservation of mass applied to the pollution abatement process, this dissertation develops a new frontier pollutant function which then is used to find corresponding marginal abatement cost of pollutants. The StoNEZD method is applied to estimate a frontier pollutant function considering the vintage of capital owned by the polluting firms. The method is applied to estimate the average NOx marginal abatement cost for the U.S. coal power plants under the current Clean Air Interstate Rule NOx program. Last, the effect of a technical change on marginal abatement costs are investigated using an index decomposition technique. The StoNEZD method is extended to estimate sequential frontier pollutant functions reflecting the innovation in pollution reduction. The method is then applied to estimate a technical change effect on a marginal abatement cost of the U.S. coal power plants under the current Clean Air Interstate Rule NOx program.

Mekaroonreung, Maethee

2012-08-01T23:59:59.000Z

194

Cosmic Ray Interactions in Shielding Materials  

SciTech Connect

This document provides a detailed study of materials used to shield against the hadronic particles from cosmic ray showers at Earth’s surface. This work was motivated by the need for a shield that minimizes activation of the enriched germanium during transport for the MAJORANA collaboration. The materials suitable for cosmic-ray shield design are materials such as lead and iron that will stop the primary protons, and materials like polyethylene, borated polyethylene, concrete and water that will stop the induced neutrons. The interaction of the different cosmic-ray components at ground level (protons, neutrons, muons) with their wide energy range (from kilo-electron volts to giga-electron volts) is a complex calculation. Monte Carlo calculations have proven to be a suitable tool for the simulation of nucleon transport, including hadron interactions and radioactive isotope production. The industry standard Monte Carlo simulation tool, Geant4, was used for this study. The result of this study is the assertion that activation at Earth’s surface is a result of the neutronic and protonic components of the cosmic-ray shower. The best material to shield against these cosmic-ray components is iron, which has the best combination of primary shielding and minimal secondary neutron production.

Aguayo Navarrete, Estanislao; Kouzes, Richard T.; Ankney, Austin S.; Orrell, John L.; Berguson, Timothy J.; Troy, Meredith D.

2011-09-08T23:59:59.000Z

195

THE SPINE OF THE COSMIC WEB  

Science Conference Proceedings (OSTI)

We present the SpineWeb framework for the topological analysis of the Cosmic Web and the identification of its walls, filaments, and cluster nodes. Based on the watershed segmentation of the cosmic density field, the SpineWeb method invokes the local adjacency properties of the boundaries between the watershed basins to trace the critical points in the density field and the separatrices defined by them. The separatrices are classified into walls and the spine, the network of filaments and nodes in the matter distribution. Testing the method with a heuristic Voronoi model yields outstanding results. Following the discussion of the test results, we apply the SpineWeb method to a set of cosmological N-body simulations. The latter illustrates the potential for studying the structure and dynamics of the Cosmic Web.

Aragon-Calvo, Miguel A.; Szalay, Alexander S. [Johns Hopkins University, 3701 San Martin Drive, Baltimore, MD 21218 (United States); Platen, Erwin; Van de Weygaert, Rien [Kapteyn Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen (Netherlands)

2010-11-01T23:59:59.000Z

196

The Spine of the Cosmic Web  

E-Print Network (OSTI)

We present the SpineWeb framework for the topological analysis of the Cosmic Web and the identification of its walls, filaments and cluster nodes. Based on the watershed segmentation of the cosmic density field, the SpineWeb method invokes the local adjacency properties of the boundaries between the watershed basins to trace the critical points in the density field and the separatrices defined by them. The separatrices are classified into walls and the spine, the network of filaments and nodes in the matter distribution. Testing the method with a heuristic Voronoi model yields outstanding results. Following the discussion of the test results, we apply the SpineWeb method to a set of cosmological N-body simulations. The latter illustrates the potential for studying the structure and dynamics of the Cosmic Web.

Miguel A. Aragon-Calvo; Erwin Platen; Rien van de Weygaert; Alexander S. Szalay

2008-09-30T23:59:59.000Z

197

Cosmic Shear from STIS Pure Parallels: Analysis  

E-Print Network (OSTI)

The measurement of cosmic shear requires deep imaging with high image quality on many lines of sight to sample the statistics of large-scale structure. The expected distortion of galaxy images by cosmic shear on the STIS angular scale is a few percent, therefore the PSF anisotropy has to be understood and controlled to an accuracy better than 1%. In this poster we present the analysis of the PSF of STIS and a preliminary cosmic shear measurement using archival data from the STIS pure parallel program to show that the STIS camera on-board HST is well suited for our project. The data reduction and catalog production are described in an accompanying paper (astro-ph/0102330).

H. Haemmerle; J. -M. Miralles; P. Schneider; T. Erben; R. A. E. Fosbury; W. Freudling; N. Pirzkal; S. D. M. White

2001-09-27T23:59:59.000Z

198

OECD energy intensity  

Science Conference Proceedings (OSTI)

to examine OECD countries' energy intensity levels (i.e., the ratio of energy ... steady-state or long-run distribution of energy intensity for the Organisation of ...

199

Cosmic string collision in cosmological backgrounds  

SciTech Connect

The collisions of cosmic string loops and the dynamics of junction formations in expanding backgrounds are studied. The key parameter controlling the dynamics of junction formation, the cosmic strings zipping and unzipping, is the relative size of the loops compared to the Hubble radius at the time of collision. We study analytically and numerically these processes for large superhorizon size loops, for small subhorizon size loops as well as for loops with the radii comparable to the Hubble radius at the time of collision.

Firouzjahi, Hassan [School of Physics, Institute for Research in Fundamental Sciences (IPM), P.O. Box 19395-5531, Tehran (Iran, Islamic Republic of); Khoeini-Moghaddam, Salomeh [School of Physics, Institute for Research in Fundamental Sciences (IPM), P.O. Box 19395-5531, Tehran (Iran, Islamic Republic of); Department of Physics, Faculty of Science, Tarbiat Mo'allem University, Tehran (Iran, Islamic Republic of); Khosravi, Shahram [Department of Physics, Faculty of Science, Tarbiat Mo'allem University, Tehran (Iran, Islamic Republic of); School of Astronomy, Institute for Research in Fundamental Sciences (IPM), P.O. Box 19395-5531, Tehran (Iran, Islamic Republic of)

2010-06-15T23:59:59.000Z

200

Cosmic Rays and Gamma Ray Bursts From Microblazars  

E-Print Network (OSTI)

Highly relativistic jets from merger and accretion induced collapse of compact stellar objects, which may produce the cosmological gamma ray bursts (GRBs), are also very efficient and powerful cosmic ray accelerators. The expected luminosity, energy spectrum and chemical composition of cosmic rays from Galactic GRBs, most of which do not point in our direction, can explain the observed properties of Galactic cosmic rays.

Arnon Dar

1998-09-13T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


201

Ultrahigh Energy Cosmic Rays: New Physics or Old Physics?  

E-Print Network (OSTI)

We consider the advantages of and the problems associated with hypotheses to explain the origin of ulthrahigh energy cosmic rays (UHECR: E > 10 EeV) and the "trans GZK" cosmic rays (TGZK: E > 100 EeV), both through "old physics" (acceleration in cosmic sources) and "new physics" (new particles, topological defects, fat neutrino cross sections, Lorentz invariance violation).

F. W. Stecker

2004-07-15T23:59:59.000Z

202

Light Matters (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'Light Matters' was submitted by the Center for Light-Material Interactions in Energy Conversion (LMI) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. This video was selected as one of five winners by a distinguished panel of judges for its 'striking photography and visual impact'. LMI, an EFRC directed by Harry Atwater at the California Institute of Technology is a partnership of scientists from three institutions: CalTech (lead), University of California, Berkeley, and the University of Illinois at Urbana-Champaign. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of Light-Material Interactions in Energy Conversion is 'to tailor the morphology, complex dielectric structure, and electronic properties of matter to sculpt the flow of sunlight, enabling light conversion to electrical and chemical energy with unprecedented efficiency.' Research topics are: catalysis (imines hydrocarbons), solar photovoltaic, solar fuels, photonic, solid state lighting, metamaterial, optics, phonons, thermal conductivity, solar electrodes, photsynthesis, CO{sub 2} (convert), greenhouse gas, and matter by design.

Atwater, Harry (Director, Light-Material Interactions in Energy Conversion (LMI), California Institute of Technology); LMI Staff

2011-05-01T23:59:59.000Z

203

Carbon in Underland (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum  

SciTech Connect

'Carbon in Underland' was submitted by the Center for Nanoscale Control of Geologic CO2 (NCGC) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. This video was selected as one of five winners by a distinguished panel of judges for its 'entertaining animation and engaging explanations of carbon sequestration'. NCGC, an EFRC directed by Donald J. DePaolo at Lawrence Berkeley National Laboratory is a partnership of scientists from seven institutions: LBNL (lead) Massachusetts Institute of Technology, Lawrence Livermore National Laboratory, Oak Ridge National Laboratory, University of California, Davis, Ohio State University, and Washington University in St. Louis. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of the Center for Nanoscale Control of Geologic CO{sub 2} is 'to use new investigative tools, combined with experiments and computer simulations, to build a fundamental understanding of molecular-to-pore-scale processes in fluid-rock systems, and to demonstrate the ability to control critical aspects of flow, transport, and mineralization in porous rock media as applied to geologic sequestration of CO{sub 2}. Research topics are: bio-inspired, CO{sub 2} (store), greenhouse gas, and interfacial characterization.

DePaolo, Donald J. (Director, Center for Nanoscale Control of Geologic CO2); NCGC Staff

2011-05-01T23:59:59.000Z

204

Solar Variability, Cosmic Rays and Climate: What's up? The topic of possible relations between solar and cosmic  

E-Print Network (OSTI)

Preface Solar Variability, Cosmic Rays and Climate: What's up? The topic of possible relations between solar and cosmic ray variability on one hand, and Earth's climate on the other hand, is quite in Space Research topical issue on Solar Variability, Cosmic Rays and Climate presents a collection

Usoskin, Ilya G.

205

Evidences of high energy protons with energies beyond 0.4 GeV in the solar particle spectrum as responsible for the cosmic rays solar diurnal anisotropy  

E-Print Network (OSTI)

Analysis on the daily variations of cosmic ray muons with $E_{\\mu}\\geq 0.2 GeV$ based on the data of two directional muon telescopes at sea level and with a rigidity of response to cosmic proton spectrum above 0.4 GV is presented. The analysis covers two months of observations and in 60% of days, abrupt transitions between a low to a high muon intensity and vice-verse is observed, the period of high muon intensity is from $\\sim 8.0h$ up to $\\sim 19.0h$ (local time) and coincides with the period when the interplanetary magnetic field (IMF) lines overtake the Earth. This behavior strongly suggest that the high muon intensity is due to a contribution of solar protons (ions) on the muon intensity produced by the galactic cosmic rays, responsible for the low muon intensity. This implies that the solar particle spectrum extends to energies beyond 1 GeV. We show that this picture can explain the solar daily variation origin, and it is a most accurate scenario than the assumption of corotating galactic cosmic ray with the IMF lines, specially in the high rigidity region. Obtained results are consistent with the data reported in others papers. Some aspects on the sensitivity of our muon telescopes are also presented.

C. E. Navia; C. R. A. Augusto; M. B. Robba; K. H. Tsui

2007-06-26T23:59:59.000Z

206

Evidences of high energy protons with energies beyond 0.4 GeV in the solar particle spectrum as responsible for the cosmic rays solar diurnal anisotropy  

E-Print Network (OSTI)

Analysis on the daily variations of cosmic ray muons with $E_{\\mu}\\geq 0.2 GeV$ based on the data of two directional muon telescopes at sea level and with a rigidity of response to cosmic proton spectrum above 0.4 GV is presented. The analysis covers two months of observations and in 60% of days, abrupt transitions between a low to a high muon intensity and vice-verse is observed, the period of high muon intensity is from $\\sim 8.0h$ up to $\\sim 19.0h$ (local time) and coincides with the period when the interplanetary magnetic field (IMF) lines overtake the Earth. This behavior strongly suggest that the high muon intensity is due to a contribution of solar protons (ions) on the muon intensity produced by the galactic cosmic rays, responsible for the low muon intensity. This implies that the solar particle spectrum extends to energies beyond 1 GeV. We show that this picture can explain the solar daily variation origin, and it is a most accurate scenario than the assumption of corotating galactic cosmic ray wit...

Navia, C E; Robba, M B; Tsui, K H

2007-01-01T23:59:59.000Z

207

Observation of an Anisotropy in the Galactic Cosmic Ray arrival direction at 400 TeV with IceCube  

E-Print Network (OSTI)

In this paper we report the first observation in the Southern hemisphere of an energy dependence in the Galactic cosmic ray anisotropy up to a few hundred TeV. This measurement was performed using cosmic ray induced muons recorded by the partially deployed IceCube observatory between May 2009 and May 2010. The data include a total of 33$\\times 10^{9}$ muon events with a median angular resolution of $\\sim3^{\\circ}$ degrees. A sky map of the relative intensity in arrival direction over the Southern celestial sky is presented for cosmic ray median energies of 20 and 400 TeV. The same large-scale anisotropy observed at median energies around 20 TeV is not present at 400 TeV. Instead, the high energy skymap shows a different anisotropy structure including a deficit with a post-trial significance of -6.3$\\sigma$. This anisotropy reveals a new feature of the Galactic cosmic ray distribution, which must be incorporated into theories of the origin and propagation of cosmic rays.

IceCube Collaboration; R. Abbasi; Y. Abdou; T. Abu-Zayyad; M. Ackermann; J. Adams; J. A. Aguilar; M. Ahlers; M. M. Allen; D. Altmann; K. Andeen; J. Auffenberg; X. Bai; M. Baker; S. W. Barwick; R. Bay; J. L. Bazo Alba; K. Beattie; J. J. Beatty; S. Bechet; J. K. Becker; K. -H. Becker; M. L. Benabderrahmane; S. BenZvi; J. Berdermann; P. Berghaus; D. Berley; E. Bernardini; D. Bertrand; D. Z. Besson; D. Bindig; M. Bissok; E. Blaufuss; J. Blumenthal; D. J. Boersma; C. Bohm; D. Bose; S. Böser; O. Botner; A. M. Brown; S. Buitink; K. S. Caballero-Mora; M. Carson; D. Chirkin; B. Christy; F. Clevermann; S. Cohen; C. Colnard; D. F. Cowen; A. H. Cruz Silva; M. V. D'Agostino; M. Danninger; J. Daughhetee; J. C. Davis; C. De Clercq; T. Degner; L. Demirörs; F. Descamps; P. Desiati; G. de Vries-Uiterweerd; T. DeYoung; J. C. Díaz-Vélez; M. Dierckxsens; J. Dreyer; J. P. Dumm; M. Dunkman; J. Eisch; R. W. Ellsworth; O. Engdegård; S. Euler; P. A. Evenson; O. Fadiran; A. R. Fazely; A. Fedynitch; J. Feintzeig; T. Feusels; K. Filimonov; C. Finley; T. Fischer-Wasels; B. D. Fox; A. Franckowiak; R. Franke; T. K. Gaisser; J. Gallagher; L. Gerhardt; L. Gladstone; T. Glüsenkamp; A. Goldschmidt; J. A. Goodman; D. Góra; D. Grant; T. Griesel; A. Groß; S. Grullon; M. Gurtner; C. Ha; A. Haj Ismail; A. Hallgren; F. Halzen; K. Han; K. Hanson; D. Heinen; K. Helbing; R. Hellauer; S. Hickford; G. C. Hill; K. D. Hoffman; B. Hoffmann; A. Homeier; K. Hoshina; W. Huelsnitz; J. -P. Hülß; P. O. Hulth; K. Hultqvist; S. Hussain; A. Ishihara; E. Jacobi; J. Jacobsen; G. S. Japaridze; H. Johansson; K. -H. Kampert; A. Kappes; T. Karg; A. Karle; P. Kenny; J. Kiryluk; F. Kislat; S. R. Klein; J. -H. Köhne; G. Kohnen; H. Kolanoski; L. Köpke; S. Kopper; D. J. Koskinen; M. Kowalski; T. Kowarik; M. Krasberg; G. Kroll; N. Kurahashi; T. Kuwabara; M. Labare; K. Laihem; H. Landsman; M. J. Larson; R. Lauer; J. Lünemann; J. Madsen; A. Marotta; R. Maruyama; K. Mase; H. S. Matis; K. Meagher; M. Merck; P. Mészáros; T. Meures; S. Miarecki; E. Middell; N. Milke; J. Miller; T. Montaruli; R. Morse; S. M. Movit; R. Nahnhauer; J. W. Nam; U. Naumann; D. R. Nygren; S. Odrowski; A. Olivas; M. Olivo; A. O'Murchadha; S. Panknin; L. Paul; C. Pérez de los Heros; J. Petrovic; A. Piegsa; D. Pieloth; R. Porrata; J. Posselt; C. C. Price; P. B. Price; G. T. Przybylski; K. Rawlins; P. Redl; E. Resconi; W. Rhode; M. Ribordy; M. Richman; J. P. Rodrigues; F. Rothmaier; C. Rott; T. Ruhe; D. Rutledge; B. Ruzybayev; D. Ryckbosch; H. -G. Sander; M. Santander; S. Sarkar; K. Schatto; T. Schmidt; A. Schönwald; A. Schukraft; A. Schultes; O. Schulz; M. Schunck; D. Seckel; B. Semburg; S. H. Seo; Y. Sestayo; S. Seunarine; A. Silvestri; G. M. Spiczak; C. Spiering; M. Stamatikos; T. Stanev; T. Stezelberger; R. G. Stokstad; A. Stößl; E. A. Strahler; R. Ström; M. Stüer; G. W. Sullivan; Q. Swillens; H. Taavola; I. Taboada; A. Tamburro; A. Tepe; S. Ter-Antonyan; S. Tilav; P. A. Toale; S. Toscano; D. Tosi; N. van Eijndhoven; J. Vandenbroucke; A. Van Overloop; J. van Santen; M. Vehring; M. Voge; C. Walck; T. Waldenmaier; M. Wallraff; M. Walter; Ch. Weaver; C. Wendt; S. Westerhoff; N. Whitehorn; K. Wiebe; C. H. Wiebusch; D. R. Williams; R. Wischnewski; H. Wissing; M. Wolf; T. R. Wood; K. Woschnagg; C. Xu; D. L. Xu; X. W. Xu; J. P. Yanez; G. Yodh; S. Yoshida; P. Zarzhitsky; M. Zoll

2011-09-05T23:59:59.000Z

208

Viscous Modified Cosmic Chaplygin Gas Cosmology  

E-Print Network (OSTI)

In this paper we construct modified cosmic Chaplygin gas which has viscosity. We use exponential function method to solve non-linear equation and obtain time-dependent dark energy density. Then discuss Hubble expansion parameter and scale factor and fix them by using observational data. We also investigate stability of this theory.

Behnam Pourhassan

2013-01-13T23:59:59.000Z

209

2Cosmic Bar Graphs Galaxy Type  

E-Print Network (OSTI)

or cosmic gamma ray bursts by other instruments in the IPN. It has also observed over 130 events which review the highlights of these observations, which include gamma-ray bursts, soft gamma repeaters Name 1.Introduction The SPI anticoincidence system was first proposed as a gamma-ray burst (GRB

210

Production of Axions by Cosmic Magnetic Helicity  

E-Print Network (OSTI)

We investigate the effects of an external magnetic helicity production on the evolution of the cosmic axion field. It is shown that a helicity larger than (few \\times 10^{-15} G)^2 Mpc, if produced at temperatures above a few GeV, is in contradiction with the existence of the axion, since it would produce too much of an axion relic abundance.

L. Campanelli; M. Giannotti

2005-12-17T23:59:59.000Z

211

Zipping and Unzipping of Cosmic String Loops in Collision  

E-Print Network (OSTI)

In this paper the collision of two cosmic string loops is studied. After collision junctions are formed and the loops are entangled. We show that after their formation the junctions start to unzip and the loops disentangle. This analysis provides a theoretical understanding of the unzipping effect observed in numerical simulations of a network of cosmic strings with more than one type of cosmic strings. The unzipping phenomena have important effects in the evolution of cosmic string networks when junctions are formed upon collision, such as in a network of cosmic superstrings.

Hassan Firouzjahi; Johanna Karouby; Shahram Khosravi; Robert Brandenberger

2009-07-28T23:59:59.000Z

212

Kaluza-Klein and Gauss-Bonnet cosmic strings  

E-Print Network (OSTI)

We make a systematic investigation of stationary cylindrically symmetric solutions to the five-dimensional Einstein and Einstein-Gauss-Bonnet equations. Apart from the five-dimensional neutral cosmic string metric, we find two new exact solutions which qualify as cosmic strings, one corresponding to an electrically charged cosmic string, the other to an extended superconducting cosmic string surrounding a charged core. In both cases, test particles are deflected away from the singular line source. We extend both kinds of solutions to exact multi-cosmic string solutions.

Mustapha Azreg-Ainou; Gérard Clément

1996-03-29T23:59:59.000Z

213

The intergalactic propagation of ultrahigh energy cosmic ray nuclei  

SciTech Connect

We investigate the propagation of ultra-high energy cosmic ray nuclei (A = 1-56) from cosmologically distant sources through the cosmic radiation backgrounds. Various models for the injected composition and spectrum and of the cosmic infrared background are studied using updated photodisintegration cross-sections. The observational data on the spectrum and the composition of ultra-high energy cosmic rays are jointly consistent with a model where all of the injected primary cosmic rays are iron nuclei (or a mixture of heavy and light nuclei).

Hooper, Dan; /Fermilab; Sarkar, Subir; /Oxford U., Theor. Phys.; Taylor, Andrew M.; /Oxford U.

2006-08-01T23:59:59.000Z

214

Probing Solar Magnetic Field with the "Cosmic-Ray Shadow" of the Sun  

E-Print Network (OSTI)

We report on a clear solar-cycle variation of the Sun's shadow in the 10 TeV cosmic-ray flux observed by the Tibet air shower array during a full solar cycle from 1996 to 2009. In order to clarify the physical implications of the observed solar cycle variation, we develop numerical simulations of the Sun's shadow, using the Potential Field Source Surface (PFSS) model and the Current Sheet Source Surface (CSSS) model for the coronal magnetic field. We find that the intensity deficit in the simulated Sun's shadow is very sensitive to the coronal magnetic field structure, and the observed variation of the Sun's shadow is better reproduced by the CSSS model. This is the first successful attempt to evaluate the coronal magnetic field models by using the Sun's shadow observed in the TeV cosmic-ray flux.

Amenomori, M; Chen, D; Chen, T L; Chen, W Y; Cui, S W; Danzengluobu,; Ding, L K; Feng, C F; Feng, Zhaoyang; Feng, Z Y; Gou, Q B; Guo, Y Q; Hakamada, K; He, H H; He, Z T; Hibino, K; Hotta, N; Hu, Haibing; Hu, H B; Huang, J; Jia, H Y; Jiang, L; Kajino, F; Kasahara, K; Katayose, Y; Kato, C; Kawata, K; Labaciren,; Le, G M; Li, A F; Li, H J; Li, W J; Liu, C; Liu, J S; Liu, M Y; Lu, H; Meng, X R; Mizutani, K; Munakata, K; Nanjo, H; Nishizawa, M; Ohnishi, M; Ohta, I; Onuma, H; Ozawa, S; Qian, X L; Qu, X B; Saito, T; Saito, T Y; Sakata, M; Sako, T K; Shao, J; Shibata, M; Shiomi, A; Shirai, T; Sugimoto, H; Takita, M; Tan, Y H; Tateyama, N; Torii, S; Tsuchiya, H; Udo, S; Wang, H; Wu, H R; Xue, L; Yamamoto, Y; Yang, Z; Yasue, S; Yuan, A F; Yuda, T; Zhai, L M; Zhang, H M; Zhang, J L; Zhang, X Y; Zhang, Y; Zhang, Yi; Zhang, Ying; Zhaxisangzhu,; Zhou, X X

2013-01-01T23:59:59.000Z

215

ULTRA-DEEPWATER AND FRONTIER REGIONS RESEARCH NETL Team Technical Coordinator: Kelly Rose  

NLE Websites -- All DOE Office Websites (Extended Search)

ULTRA-DEEPWATER AND FRONTIER REGIONS RESEARCH NETL Team Technical Coordinator: Kelly Rose ULTRA-DEEPWATER AND FRONTIER REGIONS RESEARCH NETL Team Technical Coordinator: Kelly Rose Name Project Role Affiliation University Project Title Enick, Robert PI Pitt Baled, Hseen Post Doc Pitt Enick, Robert PI Pitt Baled, Hseen Post Doc Pitt Liu, Xingbo PI WVU Chen, Ting Graduate Student WVU Enick, Robert PI Pitt Baled, Hseen Post Doc Pitt Xing, Dazun Post Doc Pitt Baled, Hseen Grad Student Pitt Anderson, Brian PI WVU Velaga, Srinath Grad Student WVU Equation of State Model Assessment and development Evaluate Heavy Oil Viscosity Standard Quantifying complex fluid- phase properties at high pressure/high temperature (HTHP) Experimental and numerical evaluation of key metal-based failures Plume Modeling for High- pressure Water Tunnel Facility Name Title Affiliation Rose, Kelly Geologist

216

Observing air showers from cosmic superluminal particles  

Science Conference Proceedings (OSTI)

The Poincare relativity principle has been tested at low energy with great accuracy, but its extrapolation to very high-energy phenomena is much less well established. Lorentz symmetry can be broken at Planck scale due to the renormalization of gravity or to some deeper structure of matter: we expect such a breaking to be a very high energy and very short distance phenomenon. If textbook special relativity is only an approximate property of the equations describing a sector of matter above some critical distance scale, an absolute local frame (the 'vacuum rest frame', VRF) can possibly be found and superluminal sectors of matter may exist related to new degrees of freedom not yet discovered experimentally. The new superluminal particles ('superbradyons', i.e. bradyons with superluminal critical speed) would have positive mass and energy, and behave kinematically like 'ordinary' particles (those with critical speed in vacuum equal to c, the speed of light) apart from the difference in critical speed (we expect c{sub i}>>c, where c{sub i} is the critical speed of a superluminal sector). They may be the ultimate building blocks of matter. At speed v>c, they are expected to release ''Cherenkov'' radiation ('ordinary' particles) in vacuum. Superluminal particles could provide most of the cosmic (dark) matter and produce very high-energy cosmic rays. We discuss: a) the possible relevance of superluminal matter to the composition, sources and spectra of high-energy cosmic rays; b) signatures and experiments allowing to possibly explore such effects. Very large volume and unprecedented background rejection ability are crucial requirements for any detector devoted to the search for cosmic superbradyons. Future cosmic-ray experiments using air-shower detectors (especially from space) naturally fulfil both requirements.

Gonzalez-Mestres, Luis [Laboratoire de Physique Corpusculaire, College de France, 75231 Paris Cedex 05 (France); L.A.P.P., CNRS-IN2P3, B.P. 110, 74941 Annecy-le-Vieux Cedex (France)

1998-06-15T23:59:59.000Z

217

Scaling HEP to Web size with RESTful protocols: The frontier example  

SciTech Connect

The World-Wide-Web has scaled to an enormous size. The largest single contributor to its scalability is the HTTP protocol, particularly when used in conformity to REST (REpresentational State Transfer) principles. High Energy Physics (HEP) computing also has to scale to an enormous size, so it makes sense to base much of it on RESTful protocols. Frontier, which reads databases with an HTTP-based RESTful protocol, has successfully scaled to deliver production detector conditions data from both the CMS and ATLAS LHC detectors to hundreds of thousands of computer cores worldwide. Frontier is also able to re-use a large amount of standard software that runs the Web: on the clients, caches, and servers. I discuss the specific ways in which HTTP and REST enable high scalability for Frontier. I also briefly discuss another protocol used in HEP computing that is HTTP-based and RESTful, and another protocol that could benefit from it. My goal is to encourage HEP protocol designers to consider HTTP and REST whenever the same information is needed in many places.

Dykstra, Dave; /Fermilab

2011-01-01T23:59:59.000Z

218

AGS intensity upgrades  

SciTech Connect

After the successful completion of the AGS Booster and several upgrades of the AGS, a new intensity record of 6.3 x 10{sup 13} protons per pulse accelerated to 24 GeV was achieved. The high intensity slow-extracted beam program at the AGS typically serves about five production targets and about eight experiments including three rare Kaon decay experiments. Further intensity upgrades are being discussed that could increase the average delivered beam intensity by up to a factor of four.

Roser, T.

1995-12-01T23:59:59.000Z

219

Light intensity compressor  

DOE Patents (OSTI)

In a system for recording images having vastly differing light intensities over the face of the image, a light intensity compressor is provided that utilizes the properties of twisted nematic liquid crystals to compress the image intensity. A photoconductor or photodiode material that is responsive to the wavelength of radiation being recorded is placed adjacent a layer of twisted nematic liquid crystal material. An electric potential applied to a pair of electrodes that are disposed outside of the liquid crystal/photoconductor arrangement to provide an electric field in the vicinity of the liquid crystal material. The electrodes are substantially transparent to the form of radiation being recorded. A pair of crossed polarizers are provided on opposite sides of the liquid crystal. The front polarizer linearly polarizes the light, while the back polarizer cooperates with the front polarizer and the liquid crystal material to compress the intensity of a viewed scene. Light incident upon the intensity compressor activates the photoconductor in proportion to the intensity of the light, thereby varying the field applied to the liquid crystal. The increased field causes the liquid crystal to have less of a twisting effect on the incident linearly polarized light, which will cause an increased percentage of the light to be absorbed by the back polarizer. The intensity of an image may be compressed by forming an image on the light intensity compressor.

Rushford, Michael C. (Livermore, CA)

1990-01-01T23:59:59.000Z

220

A MEASUREMENT OF ANISOTROPY IN THE COSMIC BACKGROUND RADIATION ON A LARGE ANGULAR SCALE AT 33 GHz  

E-Print Network (OSTI)

component, the cosmic blackbody radiation is isotropic to 1variation of the cosmic blackbody radiation Itself. c c Thisin the Cosmic Blackbody Radiation Appendix B - Radiometer

Gorenstein, M.V.

2011-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


221

The Behavior of Hydrogen Under Extreme Conditions on Ultrafast Timescales (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'The Behavior of Hydrogen Under Extreme Conditions on Ultrafast Timescales ' was submitted by the Center for Energy Frontier Research in Extreme Environments (EFree) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. EFree is directed by Ho-kwang Mao at the Carnegie Institute of Washington and is a partnership of scientists from thirteen institutions.The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of Energy Frontier Research in Extreme Environments is 'to accelerate the discovery and creation of energy-relevant materials using extreme pressures and temperatures.' Research topics are: catalysis (CO{sub 2}, water), photocatalysis, solid state lighting, optics, thermelectric, phonons, thermal conductivity, solar electrodes, fuel cells, superconductivity, extreme environment, radiation effects, defects, spin dynamics, CO{sub 2} (capture, convert, store), greenhouse gas, hydrogen (fuel, storage), ultrafast physics, novel materials synthesis, and defect tolerant materials.

Mao, Ho-kwang (Director, Center for Energy Frontier Research in Extreme Environments); EFree Staff

2011-05-01T23:59:59.000Z

222

The Cosmic Stellar Birth and Death Rates  

E-Print Network (OSTI)

The cosmic stellar birth rate can be measured by standard astronomical techniques. It can also be probed via the cosmic stellar death rate, though until recently, this was much less precise. However, recent results based on measured supernova rates, and importantly, also on the attendant diffuse fluxes of neutrinos and gamma rays, have become competitive, and a concordant history of stellar birth and death is emerging. The neutrino flux from all past core-collapse supernovae, while faint, is realistically within reach of detection in Super-Kamiokande, and a useful limit has already been set. I will discuss predictions for this flux, the prospects for neutrino detection, the implications for understanding core-collapse supernovae, and a new limit on the contribution of type-Ia supernovae to the diffuse gamma-ray background.

John F. Beacom

2006-02-05T23:59:59.000Z

223

Observation of the submillimeter cosmic background spectrum  

SciTech Connect

An experimental measurement of the spectrum of the submillimeter cosmic background radiation is described. The experiment consists of measuring the night sky emission at an altitude of 39 km, correcting for the atmospheric molecular line emission, and placing limits on the contamination from sources of continuum radiation such as the apparatus itself and the earth. The observations were made on 24 July 1974 using a fully calibrated liquid-helium-cooled balloon- borne spectrophotometer. Important features of the apparatus include a cooled antenna, a polarizing interferometer, and a germanium bolometric detector. The characterization of the spectrophotometer includes the large angle response and emission of the antenna. The calibration of the instrument and corrections to the observed sky spectrum are based on measurements made during the flight. A simple model of the molecular line emission is used to determine the atmospheric contribution. The resulting spectrum covers the frequency range from 4 to 17 cm$sup -1$ and establishes that the cosmic background radiation follows the high frequency quantum cutoff for a 3K blackbody. A blackbody temperature of 2.99/sub -.$sub 14$/$sup +$.$sup 07$/K is deduced from our data. The present status of the cosmic background observations, which span more than three decades in frequency, is analyzed and it is concluded that they are all consistent with a blackbody temperature of 2.90 +- .04K (+- 1 SIGMA). This firmly supports the Big Bang cosmological model of the universe. (auth)

Woody, D.P.

1975-11-13T23:59:59.000Z

224

Ultra High-Energy Cosmic Ray Observations  

E-Print Network (OSTI)

The year 2007 has furnished us with outstanding results about the origin of the most energetic cosmic rays: a flux suppression as expected from the GZK-effect has been observed in the data of the HiRes and Auger experiments and correlations between the positions of nearby AGN and the arrival directions of trans-GZK events have been observed by the Pierre Auger Observatory. The latter finding marks the beginning of ultra high-energy cosmic ray astronomy and is considered a major breakthrough starting to shed first light onto the sources of the most extreme particles in nature. This report summarizes those observations and includes other major advances of the field, mostly presented at the 30th International Cosmic Ray Conference held in Merida, Mexico, in July 2007. With increasing statistics becoming available from current and even terminated experiments, systematic differences amongst different experiments and techniques can be studied in detail which is hoped to improve our understanding of experimental tec...

Kampert, Karl-Heinz

2008-01-01T23:59:59.000Z

225

The Intense Radiation Gas  

E-Print Network (OSTI)

We present a new dispersion relation for photons that are nonlinearly interacting with a radiation gas of arbitrary intensity due to photon-photon scattering. It is found that the photon phase velocity decreases with increasing radiation intensity, it and attains a minimum value in the limit of super-intense fields. By using Hamilton's ray equations, a self-consistent kinetic theory for interacting photons is formulated. The interaction between an electromagnetic pulse and the radiation gas is shown to produce pulse self-compression and nonlinear saturation. Implications of our new results are discussed.

M. Marklund; P. K. Shukla; B. Eliasson

2004-10-14T23:59:59.000Z

226

Rydberg atom detection of the temporal coherence of cosmic microwave background radiation  

E-Print Network (OSTI)

Rydberg atoms immersed in cold blackbody radiation are shown to display long-lived quantum coherence effects on timescales of tens of picoseconds. By solving non-Markovian equations of motion with no free parameters we obtain the time evolution of the density matrix, and demonstrate that the blackbody-induced temporal coherences manifest as quantum beats in time-resolved fluorescence intensities of the Rydberg atoms. A measurable fluorescence signal can be obtained with a cold trapped ensemble of 1e8 Rydberg atoms subject to 2.7 K cosmic microwave background radiation (CMB), allowing for novel insights into previously unexamined quantum coherence properties of CMB.

Tscherbul, Timur V

2013-01-01T23:59:59.000Z

227

Rydberg atom detection of the temporal coherence of cosmic microwave background radiation  

E-Print Network (OSTI)

Rydberg atoms immersed in cold blackbody radiation are shown to display long-lived quantum coherence effects on timescales of tens of picoseconds. By solving non-Markovian equations of motion with no free parameters we obtain the time evolution of the density matrix, and demonstrate that the blackbody-induced temporal coherences manifest as decaying quantum beats in time-resolved fluorescence intensities of the Rydberg atoms. A measurable fluorescence signal can be obtained with a cold trapped ensemble of 10^8 Rydberg atoms subject to suitably amplified cosmic microwave background radiation (CMB) at 2.7 K, allowing for novel insights into previously unexamined quantum coherence properties of CMB.

Timur V. Tscherbul; Paul Brumer

2013-05-23T23:59:59.000Z

228

Silver isotopic anomalies in iron meteorites: cosmic-ray production and other possible sources  

Science Conference Proceedings (OSTI)

The sources of excess /sup 107/Ag observed in iron meteorites by Kaiser, Kelly, and Wasserburg (1980) are examined, with emphasis on the reactions of cosmic-ray particles with palladium. The cross sections for the production of the silver isotopes from palladium by energetic cosmic-ray particles are evaluated or estimated and used to calculate spallogenic production rates relative to that of /sup 53/Mn from iron. The upper limit for the production rate of excess /sup 107/Ag by galactic-cosmic-ray particles is 400 atoms/min/kg(Pd) which, over an exposure age of 10/sup 9/ years, would make only 1% of the observed excesses of /sup 107/Ag. Neutron-capture reactions with Pd isotopes produce mainly /sup 109/Ag. Binary fission of a siderophilic superheavy element would be expected to yield more /sup 109/Ag than /sup 107/Ag. An intense proton irradiation in the early solar system probably would produce a lower ratio of (/sup 107/Pd//sup 108/Pd) to (/sup 26/Al//sup 27/Al) than observed in meteorites. Therefore the presence of excess /sup 107/Ag in iron meteorites with large Pd/Ag ratios very likely is due to the incorporation of 6.5 x 10/sup 6/-year /sup 107/Pd of nucleosynthetic origin in these meteorites.

Reedy, R.C.

1980-04-18T23:59:59.000Z

229

The Hurricane Intensity Issue  

Science Conference Proceedings (OSTI)

The intensity issue of hurricanes is addressed in this paper using the angular momentum budget of a hurricane in storm-relative cylindrical coordinates and a scale-interaction approach. In the angular momentum budget in storm-relative coordinates,...

T. N. Krishnamurti; S. Pattnaik; L. Stefanova; T. S. V. Vijaya Kumar; B. P. Mackey; A. J. O’Shay; Richard J. Pasch

2005-07-01T23:59:59.000Z

230

NERSC Helps Discover Cosmic Transients - NERSC Science News June...  

NLE Websites -- All DOE Office Websites (Extended Search)

Lab) to expose relatively rare and fleeting cosmic events, like supernovae and gamma ray bursts. In fact, during the commissioning phase alone, the survey has already uncovered...

231

Search for Cosmic Axions using an Optical Interferometer  

E-Print Network (OSTI)

A high finesse optical cavity can be used to search for cosmic axions in the mass range 10^{-6}search.

Adrian C. Melissinos

2008-07-07T23:59:59.000Z

232

Upgrade To The Pierre Auger Cosmic Ray Observatory's Lidar System.  

E-Print Network (OSTI)

??The Pierre Auger Cosmic Ray Observatory currently operates four elastic lidar systems in order to characterize the atmospheric aerosol content above the observatory. The atmospheric… (more)

Petermann, Emily B

2010-01-01T23:59:59.000Z

233

Snowmass Energy Frontier Simulations using the Open Science Grid (A Snowmass 2013 whitepaper)  

E-Print Network (OSTI)

Snowmass is a US long-term planning study for the high-energy community by the American Physical Society's Division of Particles and Fields. For its simulation studies, opportunistic resources are harnessed using the Open Science Grid infrastructure. Late binding grid technology, GlideinWMS, was used for distributed scheduling of the simulation jobs across many sites mainly in the US. The pilot infrastructure also uses the Parrot mechanism to dynamically access CvmFS in order to ascertain a homogeneous environment across the nodes. This report presents the resource usage and the storage model used for simulating large statistics Standard Model backgrounds needed for Snowmass Energy Frontier studies.

Avetisyan, A; Narain, M; Padhi, S; Hirschauer, J; Levshina, T; McBride, P; Sehgal, C; Slyz, M; Rynge, M; Malik, S; Stupak, J

2013-01-01T23:59:59.000Z

234

Snowmass Energy Frontier Simulations using the Open Science Grid (A Snowmass 2013 whitepaper)  

E-Print Network (OSTI)

Snowmass is a US long-term planning study for the high-energy community by the American Physical Society's Division of Particles and Fields. For its simulation studies, opportunistic resources are harnessed using the Open Science Grid infrastructure. Late binding grid technology, GlideinWMS, was used for distributed scheduling of the simulation jobs across many sites mainly in the US. The pilot infrastructure also uses the Parrot mechanism to dynamically access CvmFS in order to ascertain a homogeneous environment across the nodes. This report presents the resource usage and the storage model used for simulating large statistics Standard Model backgrounds needed for Snowmass Energy Frontier studies.

A. Avetisyan; S. Bhattacharya; M. Narain; S. Padhi; J. Hirschauer; T. Levshina; P. McBride; C. Sehgal; M. Slyz; M. Rynge; S. Malik; J. Stupak III

2013-08-04T23:59:59.000Z

235

Vision to reality: From Robert R. Wilson's frontier to Leon M. Lederman's Fermilab  

E-Print Network (OSTI)

This paper examines the roles of vision and leadership in creating and directing Fermi National Accelerator Laboratory from the late 1960s through the 1980s. The story divides into two administrations having different problems and accomplishments, that of Robert R. Wilson (1967-1978), which saw the transformation from cornfield to frontier physics facility, and that of Leon Max Lederman (1979-1989), in which the laboratory evolved into one of the world's major high-energy facilities. Lederman's pragmatic vision of a user-based experimental community helped him to convert the pioneering facility that Wilson had built frugally into a laboratory with a stable scientific, cultural, and funding environment.

Hoddeson, Lillian H; 10.1007/s000160300003

2011-01-01T23:59:59.000Z

236

Extracting cosmic microwave background polarization from satelliteastrophysical maps  

Science Conference Proceedings (OSTI)

We present the application of the fast independent component analysis (FASTICA) technique for blind component separation to polarized astrophysical emission. We study how the cosmic microwave background (CMB) polarized signal, consisting of E and B modes, can be extracted from maps affected by substantial contamination from diffuse Galactic foreground emission and instrumental noise. We implement Monte Carlo chains varying the CMB and noise realizations in order to assess the average capabilities of the algorithm and their variance. We perform the analysis of all-sky maps simulated according to the Planck satellite capabilities, modeling the sky signal as a superposition of the CMB and of the existing simulated polarization templates of Galactic synchrotron. Our results indicate that the angular power spectrum of CMB E mode can be recovered on all scales up to lsimilar or equal to 1000, corresponding to the fourth acoustic oscillation, while the B-mode power spectrum can be detected, up to its turnover at lsimilar or equal to 100, if the ratio of tensor to scalar contributions to the temperature quadrupole exceeds 30 per cent. The power spectrum of the cross-correlation between total intensity and polarization, TE, can be recovered up to lsimilar or equal to 1200, corresponding to the seventh TE acoustic oscillation.

Baccigalpi, C.; Perrotta, F.; Zotti, G.D.; Smoot, G.F.; Burigana,C.; Maino, D.; Bedini, L.; Salerno, E.

2004-05-02T23:59:59.000Z

237

Extracting cosmic microwave background polarisation from satellite astrophysical maps  

E-Print Network (OSTI)

We present the application of the Fast Independent Component Analysis ({\\ica}) technique for blind component separation to polarized astrophysical emission. We study how the Cosmic Microwave Background (CMB) polarized signal, consisting of $E$ and $B$ modes, can be extracted from maps affected by substantial contamination from diffuse Galactic foreground emission and instrumental noise. {We implement Monte Carlo chains varying the CMB and noise realizations in order to asses the average capabilities of the algorithm and their variance.} We perform the analysis of all sky maps simulated according to the {\\sc Planck} satellite capabilities, modelling the sky signal as a superposition of the CMB and of the existing simulated polarization templates of Galactic synchrotron. Our results indicate that the angular power spectrum of CMB $E$-mode can be recovered on all scales up to $\\ell\\simeq 1000$, corresponding to the fourth acoustic oscillation, while the $B$-mode power spectrum can be detected, up to its turnover at $\\ell\\simeq 100$, if the ratio of tensor to scalar contributions to the temperature quadrupole exceeds 30%. The power spectrum of the cross correlation between total intensity and polarization, $TE$, can be recovered up to $\\ell\\simeq 1200$, corresponding to the seventh $TE$ acoustic oscillation.

C. Baccigalupi; F. Perrotta; G. De Zotti; G. F. Smoot; C. Burigana; D. Maino; L. Bedini; E. Salerno

2002-09-27T23:59:59.000Z

238

Large-Angular-Scale Anisotropy in the Cosmic Background Radiation  

DOE R&D Accomplishments (OSTI)

We report the results of an extended series of airborne measurements of large-angular-scale anisotropy in the 3 K cosmic background radiation. Observations were carried out with a dual-antenna microwave radiometer operating at 33 GHz (.089 cm wavelength) flown on board a U-2 aircraft to 20 km altitude. In eleven flights, between December 1976 and May 1978, the radiometer measured differential intensity between pairs of directions distributed over most of the northern hemisphere with an rms sensitivity of 47 mK Hz{sup 1?}. The measurements how clear evidence of anisotropy that is readily interpreted as due to the solar motion relative to the sources of the radiation. The anisotropy is well fit by a first order spherical harmonic of amplitude 360{+ or -}50km sec{sup -1} toward the direction 11.2{+ or -}0.5 hours of right ascension and 19 {+ or -}8 degrees declination. A simultaneous fit to a combined hypotheses of dipole and quadrupole angular distributions places a 1 mK limit on the amplitude of most components of quadrupole anisotropy with 90% confidence. Additional analysis places a 0.5 mK limit on uncorrelated fluctuations (sky-roughness) in the 3 K background on an angular scale of the antenna beam width, about 7 degrees.

Gorenstein, M. V.; Smoot, G. F.

1980-05-00T23:59:59.000Z

239

High-Energy Cosmic Ray Event Data from the Pierre Auger Cosmic Ray Observatory  

DOE Data Explorer (OSTI)

The Pierre Auger Cosmic Ray Observatory in Mendoza, Argentina is the result of an international collaboration funded by 15 countries and many different organizations. Its mission is to capture high-energy cosmic ray events or air showers for research into their origin and nature. The Pierre Auger Collaboration agreed to make 1% of its data available to the public. The ôPublic Event Explorerö is a search tool that allows users to browse or search for and display figures and data plots of events collected since 2004. The repository is updated daily, and, as of July, 2009, makes 14,055 events publicly available. The energy of a cosmic ray is measured in Exa electron volts or EeV. These event displays can be browsed in order of their energy level from 0.1 to 41.1 EeV. Each event has an individual identification number.

The event displays provide station data, cosmic ray incoming direction, various energy measurements, plots, vector-based images, and an ASCII data file.

None

240

Supersymmetry and the Cosmic Ray Positron Excess  

SciTech Connect

We explore several supersymmetric alternatives to explain predictions for the cosmic ray positron excess. Light sneutrino or neutralino LSP's, and a fine-tuned model designed to provide a delta-function input, can give adequate statistical descriptions of the reported HEAT data if non-thermal production of the relic cold dark matter density dominates and/or if"boost factors" (that could originate in uncertainties from propagation or local density fluctuations) to increase the size of the signal are included. All the descriptions can be tested at the Tevatron or LHC, and some in other WIMP detecting experiments.

Kane, Gordon L.; Wang, Lian-Tao; Wang, Ting T.

2002-02-15T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


241

Decoherence in the cosmic background radiation  

E-Print Network (OSTI)

In this paper we analyze the possibility of detecting nontrivial quantum phenomena in observations of the temperature anisotropy of the cosmic background radiation (CBR), for example, if the Universe could be found in a coherent superposition of two states corresponding to different CBR temperatures. Such observations are sensitive to scalar primordial fluctuations but insensitive to tensor fluctuations, which are therefore converted into an environment for the former. Even for a free inflaton field minimally coupled to gravity, scalar-tensor interactions induce enough decoherence among histories of the scalar fluctuations as to render them classical under any realistic probe of their amplitudes.

Mariano Franco; Esteban Calzetta

2011-03-01T23:59:59.000Z

242

Current discontinuities on superconducting cosmic strings  

Science Conference Proceedings (OSTI)

The propagation of current perturbations on superconducting cosmic strings is considered. The conditions for the existence of discontinuities similar to shock waves have been found. The formulas relating the string parameters and the discontinuity propagation speed are derived. The current growth law in a shock wave is deduced. The propagation speeds of shock waves with arbitrary amplitudes are calculated. The reason why there are no shock waves in the case of time-like currents (in the 'electric' regime) is explained; this is attributable to the shock wave instability with respect to perturbations of the string world sheet.

Troyan, E., E-mail: et@iaaru.astronautiko.org; Vlasov, Yu. V. [Moscow Institute of Physics and Technology (Russian Federation)

2011-07-15T23:59:59.000Z

243

Gravitational Field of a Spinning Cosmic String  

E-Print Network (OSTI)

We study the effect of internal space rotation on the gravitational properties of infinite straight and stationary cosmic string. From the approximate solution of Einsten equations for the spinning Q-lump string we obtain long range gravitational accelleration resembling that of a rotating massive cylindrical shell. We also compute the angular velocity of the inertial frame dragging and the angle of light deflection by the Q-lump string. Matter accretion on to spinning strings can play a role in galaxy formation when the angular velocity times the string width is comparable to the speed of light.

Eugen Simanek

2008-03-02T23:59:59.000Z

244

Cosmic acceleration and Brans-Dicke theory  

SciTech Connect

We study the accelerated expansion of the universe by exploring the Brans-Dicke parameter in different eras. For this, we take the FRW universe model with a viscous fluid (without potential) and the Bianchi type-I universe model with a barotropic fluid (with and without a potential). We evaluate the deceleration parameter and the Brans-Dicke parameter to explore cosmic acceleration. It is concluded that accelerated expansion of the universe can also be achieved for higher values of the Brans-Dicke parameter in some cases.

Sharif, M., E-mail: msharif.math@pu.edu.pk; Waheed, S. [University of the Punjab, Department of Mathematics (Pakistan)

2012-10-15T23:59:59.000Z

245

Theoretical Overview of Cosmic Microwave Background Anisotropy  

E-Print Network (OSTI)

The theoretical basis for the prediction of anisotropies in the cosmic microwave background is very well developed. Very low amplitude density and temperature perturbations produce small gravitational effects, leading to an anisotropy that is a combination of temperature fluctuations at the surface of last scattering and gravitational redshifts both at last scattering and along the path to the observer. All of the primary anisotropy can be handled by linear perturbation theory, which allows a very accurate calculation of the predicted anisotropy from different models of the Universe.

E. L. Wright

2003-05-29T23:59:59.000Z

246

Le Bail Intensity Extraction  

NLE Websites -- All DOE Office Websites (Extended Search)

Le Bail Intensity Extraction Le Bail Intensity Extraction Presentation Goal Introduce the concepts behind LeBail fitting; why it is useful and how to perform a Le Bail fit with GSAS. Format: PDF slides or a RealPlayer video of the slides with accompanying audio and a demo video that shows how a Le Bail fit is performed. Presentation Outline What is the Le Bail method? Other approaches Why use the Le Bail method? Parameter fitting with Le Bail intensity extraction Le Bail refinement strategies Avoiding problems with background fitting: BKGEDIT Demo: an example Le Bail fit Links Le Bail lecture Slides (as PDF file) FlashMovie presentation with index (best viewed with 1024x768 or better screen resolution) FlashMovie file (800x600 pixels) Le Bail demo FlashMovie presentation with index (best viewed with 1024x768 or

247

Adhesion and the Geometry of the Cosmic Web  

E-Print Network (OSTI)

We present a new way to formulate the geometry of the Cosmic Web in terms of Lagrangian space. The Adhesion model has an ingenious geometric interpretation out of which the spine of the Cosmic Web emerges naturally. Within this context we demonstrate a deep connection of the relation between Eulerian and Lagrangian space with that between Voronoi and Delaunay tessellations.

Johan Hidding; Rien van de Weygaert; Gert Vegter; Bernard J. T. Jones

2012-11-22T23:59:59.000Z

248

High intensity hadron accelerators  

SciTech Connect

This rapporteur report consists mainly of two parts. Part I is an abridged review of the status of all High Intensity Hadron Accelerator projects in the world in semi-tabulated form for quick reference and comparison. Part II is a brief discussion of the salient features of the different technologies involved. The discussion is based mainly on my personal experiences and opinions, tempered, I hope, by the discussions I participated in in the various parallel sessions of the workshop. In addition, appended at the end is my evaluation and expression of the merits of high intensity hadron accelerators as research facilities for nuclear and particle physics.

Teng, L.C.

1989-05-01T23:59:59.000Z

249

The Energy Spectra and Relative Abundances of Electrons and Positrons in the Galactic Cosmic Radiation  

E-Print Network (OSTI)

Observations of cosmic-ray electrons and positrons have been made with a new balloon-borne detector, HEAT (the "High-Energy Antimatter Telescope"), first flown in 1994 May from Fort Sumner, NM. We describe the instrumental approach and the data analysis procedures, and we present results from this flight. The measurement has provided a new determination of the individual energy spectra of electrons and positrons from 5 GeV to about 50 GeV, and of the combined "all-electron" intensity (e+ + e-) up to about 100 GeV. The single power-law spectral indices for electrons and positrons are alpha = 3.09 +/- 0.08 and 3.3 +/- 0.2, respectively. We find that a contribution from primary sources to the positron intensity in this energy region, if it exists, must be quite small.

S. W. Barwick; J. J. Beatty; C. R. Bower; C. J. Chaput; S. Coutu; G. A. de Nolfo; M. A. DuVernois; D. Ellithorpe; D. Ficenec; J. Knapp; D. M. Lowder; S. McKee; D. Muller; J. A. Musser; S. L. Nutter; E. Schneider; S. P. Swordy; G. Tarle; A. D. Tomasch; E. Torbet

1997-12-24T23:59:59.000Z

250

On the significance of the observed clustering of ultra-high energy cosmic rays  

E-Print Network (OSTI)

Three pairs of possibly correlated ultra-high energy cosmic ray events were reported by Hayashida et al (1996). Here we calculate the propagation of the corresponding particles through both the intergalactic and galactic magnetic fields. The large scale disc and halo magnetic components are approximated by the models of Stanev (1997). The intergalactic magnetic field intensity is modulated by the actual density of luminous matter along the corresponding lines of sight, calculated from the CfA redshift catalogue (Huchra et al, 1995). The results indicate that, if the events of each pair had a common source and were simultaneously produced, they either originated inside the galactic halo or otherwise very unlikely events were observed. On the other hand, an estimate of the arrival probability of ultra-high energy cosmic rays, under the assumption that the distribution of luminous matter in the nearby universe traces the distribution of the sources of the particles and intensity of the intergalactic magnetic field, suggests that the pairs are chance clusterings.

Gustavo A. Medina Tanco

1998-01-08T23:59:59.000Z

251

Precision monitoring of relative beam intensity for Mu2e  

SciTech Connect

For future experiments at the intensity frontier, precise and accurate knowledge of beam time structure will be critical to understanding backgrounds. The proposed Mu2e experiment will utilize {approx}200 ns (FW) bunches of 3 x 10{sup 7} protons at 8 GeV with a bunch-to-bunch period of 1695 ns. The out-of-bunch beam must be suppressed by a factor of 10{sup -10} relative to in-bunch beam and continuously monitored. I propose a Cerenkov-based particle telescope to measure secondary production from beam interactions in a several tens of microns thick foil. Correlating timing information with beam passage will allow the determination of relative beam intensity to arbitrary precision given a sufficiently long integration time. The goal is to verify out-of-bunch extinction to the level 10{sup -6} in the span of several seconds. This will allow near real-time monitoring of the initial extinction of the beam resonantly extracted from Fermilabs Debuncher before a system of AC dipoles and collimators, which will provide the final extinction. The effect on beam emittance is minimal, allowing the necessary continuous measurement. I will present the detector design and some concerns about bunch growth during the resonant extraction.

Evans, N.J.; Kopp, S.E.; /Texas U.; Prebys, E.; /Fermilab

2011-04-01T23:59:59.000Z

252

Theoretical cosmic Type Ia supernova rates  

E-Print Network (OSTI)

The aim of this work is the computation of the cosmic Type Ia supernova rates at very high redshifts (z>2). We adopt various progenitor models in order to predict the number of explosions in different scenarios for galaxy formation and to check whether it is possible to select the best delay time distribution model, on the basis of the available observations of Type Ia supernovae. We also computed the Type Ia supernova rate in typical elliptical galaxies of different initial luminous masses and the total amount of iron produced by Type Ia supernovae in each case. It emerges that: it is not easy to select the best delay time distribution scenario from the observational data and this is because the cosmic star formation rate dominates over the distribution function of the delay times; the monolithic collapse scenario predicts an increasing trend of the SN Ia rate at high redshifts whereas the predicted rate in the hierarchical scheme drops dramatically at high redshift; for the elliptical galaxies we note that the predicted maximum of the Type Ia supernova rate depends on the initial galactic mass. The maximum occurs earlier (at about 0.3 Gyr) in the most massive ellipticals, as a consequence of downsizing in star formation. We find that different delay time distributions predict different relations between the Type Ia supernova rate per unit mass at the present time and the color of the parent galaxies and that bluer ellipticals present higher supernova Type Ia rates at the present time.

R. Valiante; F. Matteucci; S. Recchi; F. Calura

2008-07-15T23:59:59.000Z

253

Cosmic String constraints from WMAP and SPT  

E-Print Network (OSTI)

The predictions of the inflationary LCDM paradigm match today's high-precision measurements of the cosmic microwave background anisotropy with remarkable precision. The same data put tight limits on other sources of anisotropy. Cosmic strings are a particularly interesting alternate source to constrain. Strings are topological defects, remnants of inflationary-era physics that persist after the big bang. They are formed in a variety of models of inflation, including popular string theory models such as brane inflation. In this paper, we show that measurements of temperature anisotropy by the South Pole Telescope break a parameter degeneracy in the WMAP data, permitting us to place a strong upper limit on the possible string contribution to the CMB anisotropy: the power sourced by zero-width strings must be <1.75% (95% CL) of the total. In the model we use, this translates to an upper limit on the string tension of Gmu < 1.7x10^{-7}. These limits imply that the best hope for detecting strings in the CMB ...

Dvorkin, Cora; Hu, Wayne

2011-01-01T23:59:59.000Z

254

Energy Intensity Strategy  

E-Print Network (OSTI)

Our presentation will cover how we began the journey of conserving energy at our facility. We’ll discuss a basic layout of our energy intensity plan and the impact our team has had on the process, what tools we’re using, what goals have been identified, how we structured the plan to include our team in the process and so on.

Rappolee, D.

2008-01-01T23:59:59.000Z

255

Unique Aspects and Scientific Challenges | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Unique Aspects and Scientific Challenges Unique Aspects and Scientific Challenges High Energy Physics (HEP) HEP Home About Research Snowmass / P5 Planning Process Intensity Frontier Cosmic Frontier Cosmic Frontier: More Information Unique Aspects and Scientific Challenges Theoretical Physics Advanced Technology R&D Accelerator R&D Stewardship Research Highlights .pdf file (13.1MB) Questions for the Universe Accomplishments Facilities Science Highlights Benefits of HEP Funding Opportunities Advisory Committees News & Resources Contact Information High Energy Physics U.S. Department of Energy SC-25/Germantown Building 1000 Independence Ave., SW Washington, DC 20585 P: (301) 903-3624 F: (301) 903-2597 E: sc.hep@science.doe.gov More Information » Cosmic Frontier Unique Aspects and Scientific Challenges

256

CIM - compact intensity modulation.  

SciTech Connect

Compact intensity modulation (CIM), a new method to modulate the intensity of a neutron beam is demonstrated. CIM allows the production of arbitrary signals where the focus point can be chosen and changed without any constraints. A novel feature in this technique compared to spin echo techniques is that the neutron polarization is kept parallel or anti-parallel to the static fields during the passage through the magnetic fields and the beating pattern at the detector is produced by an amplitude modulation (AM) of the adiabatic RF-spin flippers rather than Larmor precession like in neutron spin echo (NSE) instruments; thus, the achievable contrast is very high and the instrument resolution can be changed very quickly. This gives the fascinating possibility at pulsed neutron sources to sweep the modulation frequency of the flippers in order to increase dynamic resolution range during the same neutron pulse.

Bleuel, M.; Lang, E.; Gahler, G.; Lal, J.; Intense Pulsed Neutron Source; Inst. Lau Langevin

2008-07-21T23:59:59.000Z

257

Unlocking energy intensive habits  

NLE Websites -- All DOE Office Websites (Extended Search)

energy intensive habits energy intensive habits Presentation at LBL Oct 10, 2013 by Hal Wilhite Professor and Research Director University of Oslo Centre for Development and the Environment Source: WWF US EIA Outlook 2011 Conventional framing of the energy consumption and savings * Sovereign consumers * Economically rational and persistentely reflexive. * Uninfluenced by social and material conditions of everyday life * Focus on efficiency and not on size and volume which is for the most part treated as an indifferent variable Cognitive reductionism The change of frame * From individual to socio-material * From rational/reflexive experience-based (practical) knowledge * From efficiency to reduction A theory of habit * Acknowledges the role of lived experience (history, both cultural and personal) in forming

258

NEUTRON FLUX INTENSITY DETECTION  

DOE Patents (OSTI)

A method of measuring the instantaneous intensity of neutron flux in the core of a nuclear reactor is described. A target gas capable of being transmuted by neutron bombardment to a product having a resonance absorption line nt a particular microwave frequency is passed through the core of the reactor. Frequency-modulated microwave energy is passed through the target gas and the attenuation of the energy due to the formation of the transmuted product is measured. (AEC)

Russell, J.T.

1964-04-21T23:59:59.000Z

259

Intense ion beam generator  

DOE Patents (OSTI)

Methods and apparatus for producing intense megavolt ion beams are disclosed. In one embodiment, a reflex triode-type pulsed ion accelerator is described which produces ion pulses of more than 5 kiloamperes current with a peak energy of 3 MeV. In other embodiments, the device is constructed so as to focus the beam of ions for high concentration and ease of extraction, and magnetic insulation is provided to increase the efficiency of operation.

Humphries, Jr., Stanley (Ithaca, NY); Sudan, Ravindra N. (Ithaca, NY)

1977-08-30T23:59:59.000Z

260

The SDSS Coadd: Cosmic Shear Measurement  

Science Conference Proceedings (OSTI)

Stripe 82 in the Sloan Digital Sky Survey was observed multiple times, allowing deeper images to be constructed by coadding the data. Here we analyze the ellipticities of background galaxies in this 275 square degree region, searching for evidence of distortions due to cosmic shear. The E-mode is detected in both real and Fourier space with > 5-{sigma} significance on degree scales, while the B-mode is consistent with zero as expected. The amplitude of the signal constrains the combination of the matter density {Omega}{sub m} and fluctuation amplitude {sigma}{sub 8} to be {Omega}{sub m}{sup 0.7} {sigma}{sub 8} = 0.276{sub -0.050}{sup +0.036}.

Lin, Huan; /Fermilab; Dodelson, Scott; /Fermilab /Chicago U., EFI /Chicago U., KICP; Seo, Hee-Jong; /UC, Berkeley; Soares-Santos, Marcelle; /Fermilab; Annis, James; /Fermilab; Hao, Jiangang; /Fermilab; Johnston, David; /Fermilab; Kubo, Jeffrey M.; /Fermilab; Reis, Ribamar R.R.; /Fermilab /Rio de Janeiro Federal U.; Simet, Melanie; /Chicago U., EFI /Chicago U., KICP

2011-11-01T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
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261

Muon Acceleration in Cosmic-ray Sources  

E-Print Network (OSTI)

Many models of ultra-high energy cosmic-ray production involve acceleration in linear accelerators located in Gamma-Ray Bursts magnetars, or other sources. These source models require very high accelerating gradients, $10^{13}$ keV/cm, with the minimum gradient set by the length of the source. At gradients above 1.6 keV/cm, muons produced by hadronic interactions undergo significant acceleration before they decay. This acceleration hardens the neutrino energy spectrum and greatly increases the high-energy neutrino flux. We rule out many models of linear acceleration, setting strong constraints on plasma wakefield accelerators and on models for sources like Gamma Ray Bursts and magnetars.

Spencer R. Klein; Rune Mikkelsen; Julia K. Becker Tjus

2012-08-09T23:59:59.000Z

262

The Science Case for An Electron-Ion Collider: The Next QCD Frontier  

NLE Websites -- All DOE Office Websites (Extended Search)

Case for Case for An Electron-Ion Collider: The Next QCD Frontier Jianwei Qiu Brookhaven National Laboratory NSAC Subcommittee Meeting on Scientific Facilities February 15-16, 2013 for both BNL and JLab EIC efforts, ... 1 White Paper for the Electron-Ion Collider ELIC (JLab) eRHIC (BNL) 2 arXiv:1212.1701 Community effort and commitment Ten-week program (9/13-11/19, 2010) at Institute for Nuclear Theory (INT Report: arXiv:1108.1713v2, 500+ pages)  Many workshops on EIC physics: 3  Commitment from BNL and JLab:  EICAC - jointly by BNL and JLab  BNL EIC Task force (https://wiki.bnl.gov/eic/index.php/Main_Page)  EIC@JLab (https://eic.jlab.org/wiki/index.php/Main_Page)  Detector R&D (https://wiki.bnl.gov/conferences/index.php/EIC_R%25D)

263

The impact of trade costs on rare earth exports : a stochastic frontier estimation approach.  

SciTech Connect

The study develops a novel stochastic frontier modeling approach to the gravity equation for rare earth element (REE) trade between China and its trading partners between 2001 and 2009. The novelty lies in differentiating betweenbehind the border' trade costs by China and theimplicit beyond the border costs' of China's trading partners. Results indicate that the significance level of the independent variables change dramatically over the time period. While geographical distance matters for trade flows in both periods, the effect of income on trade flows is significantly attenuated, possibly capturing the negative effects of financial crises in the developed world. Second, the total export losses due tobehind the border' trade costs almost tripled over the time period. Finally, looking atimplicit beyond the border' trade costs, results show China gaining in some markets, although it is likely that some countries are substituting away from Chinese REE exports.

Sanyal, Prabuddha; Brady, Patrick Vane; Vugrin, Eric D.

2013-09-01T23:59:59.000Z

264

The impact of trade costs on rare earth exports : a stochastic frontier estimation approach.  

Science Conference Proceedings (OSTI)

The study develops a novel stochastic frontier modeling approach to the gravity equation for rare earth element (REE) trade between China and its trading partners between 2001 and 2009. The novelty lies in differentiating betweenbehind the border' trade costs by China and theimplicit beyond the border costs' of China's trading partners. Results indicate that the significance level of the independent variables change dramatically over the time period. While geographical distance matters for trade flows in both periods, the effect of income on trade flows is significantly attenuated, possibly capturing the negative effects of financial crises in the developed world. Second, the total export losses due tobehind the border' trade costs almost tripled over the time period. Finally, looking atimplicit beyond the border' trade costs, results show China gaining in some markets, although it is likely that some countries are substituting away from Chinese REE exports.

Sanyal, Prabuddha; Brady, Patrick Vane; Vugrin, Eric D.

2013-09-01T23:59:59.000Z

265

Cosmic Strings in the Universe: Achievements and prospects of research  

Science Conference Proceedings (OSTI)

Cosmic strings are linear structures of cosmological scales whose search has been actively conducted in recent years. Progress in constructing theoretical models and investigating the properties of cosmic strings and a significant growth of observational resources provide extensive possibilities for the search of such objects by several independent observational methods. These methods include searching for the events of gravitational lensing of distant background sources by strings and searching for the distinctive cosmic micro-wave background anisotropy structures induced by strings. We discuss these techniques and propose the methods of searching for strings oriented toward the latest spacecraft, including the Planck project.

Sazhina, O. S., E-mail: tedeshka@mail.ru; Sazhin, M. V., E-mail: moimaitre@mail.ru [Sternberg Astronomical Institute (Russian Federation)

2011-11-15T23:59:59.000Z

266

Cosmic age problem revisited in the holographic dark energy model  

E-Print Network (OSTI)

Because of an old quasar APM 08279 + 5255 at $z=3.91$, some dark energy models face the challenge of the cosmic age problem. It has been shown by Wei and Zhang [Phys. Rev. D {\\bf 76}, 063003 (2007)] that the holographic dark energy model is also troubled with such a cosmic age problem. In order to accommodate this old quasar and solve the age problem, we propose in this paper to consider the interacting holographic dark energy in a non-flat universe. We show that the cosmic age problem can be eliminated when the interaction and spatial curvature are both involved in the holographic dark energy model.

Cui, Jinglei

2010-01-01T23:59:59.000Z

267

The Revival of Galactic Cosmic Ray Nucleosynthesis?  

E-Print Network (OSTI)

Because of the roughly linear correlation between Be/H and Fe/H in low metallicity halo stars, it has been argued that a ``primary'' component in the nucleosynthesis of Be must be present in addition to the ``secondary'' component from standard Galactic cosmic ray nucleosynthesis. In this paper we critically re-evaluate the evidence for the primary versus secondary character of Li, Be, and B evolution, analyzing both in the observations and in Galactic chemical evolution models. While it appears that [Be/H] versus [Fe/H] has a logarithmic slope near 1, it is rather the Be-O trend that directly arises from the physics of spallation production. Using new abundances for oxygen in halo stars based on UV OH lines, we find that the Be-O slope has a large uncertainty due to systematic effects, rendering it difficult to distinguish from the data between the secondary slope of 2 and the primary slope of 1. The possible difference between the Be-Fe and Be-O slopes is a consequence of the variation in O/Fe versus Fe: recent data suggests a negative slope rather than zero (i.e., Fe $\\propto$ O) as is often assumed. In addition to a phenomenological analysis of Be and B evolution, we have also examined the predicted LiBeB, O, and Fe trends in Galactic chemical evolution models which include outflow. Based on our results, it is possible that a good fit to the LiBeB evolution requires only traditional the Galactic cosmic ray spallation, and the (primary) neutrino-process contribution to B11. We thus suggest that these two processes might be sufficient to explain Li6, Be, and B evolution in the Galaxy, without the need for an additional primary source of Be and B.

Brian D. Fields; Keith A. Olive

1998-09-22T23:59:59.000Z

268

Searching for Cosmic Accelerators via IceCube  

NLE Websites -- All DOE Office Websites (Extended Search)

Searching for Cosmic Searching for Cosmic Accelerators via IceCube Searching for Cosmic Accelerators via IceCube Berkeley Lab Researchers Part of an International Hunt November 21, 2013 Lynn Yarris, lcyarris@lbl.gov, 510.486.5375 Bert.jpg This event display shows "Bert," one of two neutrino events discovered at IceCube whose energies exceeded one petaelectronvolt (PeV). The colors show when the light arrived, with reds being the earliest, succeeded by yellows, greens and blues. The size of the circle indicates the number of photons observed. (Courtesy of IceCube Lab) In our universe there are particle accelerators 40 million times more powerful than the Large Hadron Collider (LHC) at CERN. Scientists don't know what these cosmic accelerators are or where they are located, but new

269

Cosmic ray lithium isotope measurement with AMS-01  

E-Print Network (OSTI)

The AMS-01 detector measured charged cosmic rays during 10 days on the Space Shuttle Discovery in 1998 and collected 108 events. By identifying 8349 Lithium and 22709 Carbon nuclei from the raw data, this thesis presents ...

Zhou, Feng, Ph. D. Massachusetts Institute of Technology

2009-01-01T23:59:59.000Z

270

Detectors of Cosmic Rays, Gamma Rays, and Neutrinos  

SciTech Connect

We summarize the main features, properties and performances of the typical detectors in use in Cosmic Ray Physics. A brief historical and general introduction will focus on the main classes and requirements of such detectors.

Altamirano, A. [Departamento de Fisica, Informatica y Matematicas, Facultad de Ciencias y Filosofia, Universidad Peruana Cayetano Heredia (Peru); Centro de Tecnologias de Informacion y Comunicaciones (CTIC), Universidad Nacional de Ingenieria, Lima (Peru); Navarra, G. [Dipartimento di Fisica Generale dell'Universita' and INFN, Torino (Italy)

2009-04-30T23:59:59.000Z

271

Searching for Cosmic Accelerators via IceCube  

NLE Websites -- All DOE Office Websites (Extended Search)

universe there are particle accelerators 40 million times more powerful than the Large Hadron Collider (LHC) at CERN. Scientists don't know what these cosmic accelerators are or...

272

Acceleration of the cosmic expansion induced by symmetry breaking  

E-Print Network (OSTI)

It is proved that in order to obtain a model of the accelerated cosmic expansion the thing one only need to do is to add a perturbation term to the Einstein-Hilbert Lagrangian. This term leads to some symmetry breaking terms in the fields equation, which makes the cosmic expansion accelerating. A vacuum de Sitter solution is obtained. A new explanation of the acceleration of the cosmic expansion is presented. In this model the changing of the expansion from decelerating to accelerating is an intrinsic property of the universe without need of an exotic dark energy. The acceleration of the cosmic expansion is induced by the symmetry breaking perturbation of the gravitational energy. The cosmological constant problem, the coincidence problem and the problem of phantom divide line crossing are naturally solved. The results of the model are roughly consistent with the observations.

G. Y. Chee

2013-01-21T23:59:59.000Z

273

Closest Type Ia Supernova in Decades Solves a Cosmic Mystery  

NLE Websites -- All DOE Office Websites (Extended Search)

use to measure cosmic growth, a technique that in 1998 led to the discovery of dark energy - and 13 years later to a Nobel Prize, "for the discovery of the accelerating...

274

Chemical Composition of Galactic Cosmic Rays with Space Experiments  

E-Print Network (OSTI)

The origin and properties of the cosmic radiation are one of the most intriguing question in modern astrophysics. The precise measurement of the chemical composition and energy spectra of the cosmic rays provides fundamental insight into these subjects. In this paper we will review the existing experimental data. Specifically, we will analyse results collected by space-born experiments discussing the experimental uncertainties and challenges with a focus on the PAMELA experiment.

Mirko Boezio; Emiliano Mocchiutti

2012-08-07T23:59:59.000Z

275

Recombination Softening and Reheating of the Cosmic Plasma  

E-Print Network (OSTI)

The atomic recombination process leads to a softening of the matter equation of state as reflected by a reduced generalized adiabatic index, with accompanying heat release. We study the effects of this recombination softening and reheating of the cosmic plasma on the ionization history, visibility function, Cold Dark Matter (CDM) transfer function, and the Cosmic Microwave Background (CMB) spectra. The resulting modifications of the CMB spectra are not negligible and should be implemented when data with higher accuracy are analysed.

Leung, P K; Chu, M C; Leung, Po Kin; Chan, Chi-Wang; Chu, Ming-Chung

2004-01-01T23:59:59.000Z

276

Cosmic Strings in a Braneworld Theory with Metastable Gravitons  

E-Print Network (OSTI)

If the graviton possesses an arbitrarily small (but nonvanishing) mass, perturbation theory implies that cosmic strings have a nonzero Newtonian potential. Nevertheless in Einstein gravity, where the graviton is strictly massless, the Newtonian potential of a cosmic string vanishes. This discrepancy is an example of the van Dam--Veltman--Zakharov (VDVZ) discontinuity. We present a solution for the metric around a cosmic string in a braneworld theory with a graviton metastable on the brane. This theory possesses those features that yield a VDVZ discontinuity in massive gravity, but nevertheless is generally covariant and classically self-consistent. Although the cosmic string in this theory supports a nontrivial Newtonian potential far from the source, one can recover the Einstein solution in a region near the cosmic string. That latter region grows as the graviton's effective linewidth vanishes (analogous to a vanishing graviton mass), suggesting the lack of a VDVZ discontinuity in this theory. Moreover, the presence of scale dependent structure in the metric may have consequences for the search for cosmic strings through gravitational lensing techniques.

Arthur Lue

2001-11-20T23:59:59.000Z

277

A Method for Constraining Cosmic Magnetic Field Models Using Ultra-High Energy Cosmic Rays: The Field Scan Method  

E-Print Network (OSTI)

The Galactic magnetic field, locally observed to be on the order of a few $\\mu$G, is sufficiently strong to induce deflections in the arrival directions of ultra-high energy cosmic rays. We present a method that establishes measures of self-consistency for hypothesis sets comprised of cosmic magnetic field models and ultra-high energy cosmic ray composition and source distributions. The method uses two independent procedures to compare the backtracked velocity vectors outside the magnetic field model to the distribution of backtracked velocity directions of many isotropic observations with the same primary energies. This allows for an estimate of the statistical consistency between the observed data and simulated isotropic observations. Inconsistency with the isotropic expectation of source correlation in both procedures is interpreted as the hypothesis set providing a self-consistent description of GMF and UHECR properties for the cosmic ray observations.

Michael S. Sutherland; Brian M. Baughman; James J. Beatty

2012-07-06T23:59:59.000Z

278

Autonomic Materials for Smarter, Safer, Longer-Lasting Batteries (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'Autonomic Materials for Smarter, Safer, Longer-Lasting Batteries' was submitted by the Center for Electrical Energy Storage (CEES) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. CEES, an EFRC directed by Michael Thackery at Argonne National Laboratory is a partnership of scientists from three institutions: ANL (lead), Northwestern University, and the University of Illinois at Urbana-Champaign. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of the Center for Electrical Energy Storage is 'to acquire a fundamental understanding of interfacial phenomena controlling electrochemical processes that will enable dramatic improvements in the properties and performance of energy storage devices, notable Li ion batteries.' Research topics are: electrical energy storage, batteries, battery electrodes, electrolytes, adaptive materials, interfacial characterization, matter by design; novel materials synthesis, charge transport, and defect tolerant materials.

Thackeray, Michael (Director, Center for Electrical Energy Storage); CEES Staff

2011-05-01T23:59:59.000Z

279

The Center for Material Science of Nuclear Fuel (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

Science Conference Proceedings (OSTI)

'The Center for Material Science of Nuclear Fuel (CMSNF)' was submitted by the CMSNF to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. CMSNF, an EFRC directed by Todd Allen at the Idaho National Laboratory is a partnership of scientists from six institutions: INL (lead), Colorado School of Mines, University of Florida, Florida State University, Oak Ridge National Laboratory, and the University of Wisconsin at Madison. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of the Center for Materials Science of Nuclear Fuels is 'to achieve a first-principles based understanding of the effect of irradiation-induced defects and microstructures on thermal transport in oxide nuclear fuels.' Research topics are: phonons, thermal conductivity, nuclear, extreme environment, radiation effects, defects, and matter by design.

Allen, Todd (Director, Center for Material Science of Nuclear Fuel); CMSNF Staff

2011-05-01T23:59:59.000Z

280

Center for Materials at Irradiation and Mechanical Extremes at LANL (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

Science Conference Proceedings (OSTI)

'Center for Materials at Irradiation and Mechanical Extremes (CMIME) at LANL' was submitted by CMIME to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. CMIME, an EFRC directed by Michael Nastasi at Los Alamos National Laboratory is a partnership of scientists from four institutions: LANL (lead), Carnegia Mellon University, the University of Illinois at Urbana Champaign, and the Massachusetts Institute of Technology. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges.

Michael Nastasi (Director, Center for Materials at Irradiation and Mechanical Extremes); CMIME Staff

2011-05-01T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


281

Solar Cells from Plastics? Mission Possible at the PHaSE Energy Research Center, UMass Amherst (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'Solar Cells from Plastics? Mission Possible at the PHaSE Energy Research Center, UMass Amherst' was submitted by the Polymer-Based Materials for Harvesting Solar Energy (PHaSE) EFRC to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. PHaSE, an EFRC co-directed by Thomas P. Russell and Paul M. Lahti at the University of Massachusetts, Amherst, is a partnership of scientists from six institutions: UMass (lead), Oak Ridge National Laboratory, Pennyslvania State University, Rensselaer Polytechnic Institute, and the University of Pittsburgh. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges.

Russell, Thomas P; Lahti, Paul M. (PHaSE - Polymer-Based Materials for Harvesting Solar Energy); PHaSE Staff

2011-05-01T23:59:59.000Z

282

Undergraduate Research at the Center for Energy Efficient Materials (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum  

DOE Green Energy (OSTI)

'Undergraduate Research at the Center for Energy Efficient Materials (CEEM)' was submitted by CEEM to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. CEEM, an EFRC directed by John Bowers at the University of California, Santa Barbara is a partnership of scientists from four institutions: UC, Santa Barbara (lead), UC, Santa Cruz, Los Alamos National Laboratory, and National Renewable Energy Laboratory. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of the Center for Energy Efficient Materials is 'to discover and develop materials that control the interactions between light, electricity, and heat at the nanoscale for improved solar energy conversion, solid-state lighting, and conversion of heat into electricity.' Research topics are: solar photovoltaic, photonic, solid state lighting, optics, thermoelectric, bio-inspired, electrical energy storage, batteries, battery electrodes, novel materials synthesis, and scalable processing.

Bowers, John (Director, Center for Energy Efficient Materials ); CEEM Staff

2011-05-01T23:59:59.000Z

283

CABS: Green Energy for Our Nation's Future (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

SciTech Connect

'CABS: Green Energy for our Nation's Future' was submitted by the Center for Advanced Biofuel Systems (CABS) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. CABS, an EFRC directed by Jan Jaworski at the Donald Danforth Plant Science Center is a partnership of scientists from five institutions: Donald Danforth Plant Science Center (lead), Michigan State University, the University of Nebraska, New Mexico Consortium/LANL, and Washington State University. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges.

Jan Jaworski (Director, Center for Advanced Biofuel Systems); Sayre, Richard T. (previous Director); CABS Staff

2011-05-01T23:59:59.000Z

284

Moving from Petroleum to Plants to Energize our World (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'Moving from Petroleum to Plants to Energize our World' was submitted by the Center for Direct Catalytic Conversion of Biomass to Biofuels (C3Bio) to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. C3Bio, an EFRC directed by Maureen McCann at Purdue University is a partnership between five institutions: Purdue (lead), Argonne National Laboratory, National Renewable Energy Laboratory, Northeastern University, and the University of Tennessee. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges.

McCann, Maureen (Director, Center for Direct Catalytic Conversion of Biomass to Biofuels); C3Bio Staff

2011-05-01T23:59:59.000Z

285

Gravitational Waves from Light Cosmic Strings: Backgrounds and Bursts with Large Loops  

E-Print Network (OSTI)

The mean spectrum and burst statistics of gravitational waves produced by a cosmological population of cosmic string loops are estimated using analytic approximations, calibrated with earlier simulations. Formulas are derived showing the dependence of observables on the string tension, in the regime where newly-formed loops are relatively large, not very much smaller than the horizon. Large loops form earlier, are more abundant, and generate a more intense stochastic background and more frequent bursts than assumed in earlier background estimates, enabling experiments to probe lighter cosmic strings of interest to string theory. Predictions are compared with instrument noise from current and future experiments, and with confusion noise from known astrophysical gravitational wave sources such as stellar and massive black hole binaries. In these large-loop models, current data from millisecond pulsar timing already suggests that the tension is less than about $10^{-10}$, a typical value expected in strings from brane inflation. LISA will be sensitive to stochastic backgrounds created by strings as light as $G\\mu\\approx 10^{-15}$, at frequencies where it is limited by confusion noise of Galactic stellar populations; however, for those lightest detectable strings, bursts are rarely detectable.

Craig J. Hogan

2006-05-22T23:59:59.000Z

286

343. Document entitled "Develop "Frontier" Resources to Ensure Future Oil and Na  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

3. Document entitled "Develop "Frontier" Resources to Ensure Future Oil and Natural Gas 3. Document entitled "Develop "Frontier" Resources to Ensure Future Oil and Natural Gas Supply," dated March 8, 2001. B-5 Exemption - Information withheld (under Exemption 5) consists of deliberative material reflecting comments, recommendations and revisions of draft documents relating to NEPDG. 2 pages. #4139-4140 Withheld 344. Document entitled "The Northeast Home Heating Oil Reserve," dated March 7, 2001. B-5 Exemption - Information withheld (under Exemption 5) consists of deliberative material reflecting comments, recommendations and revisions of draft documents relating to NEPDG. 2 pages. #4141-4142 Withheld 345. Document entitled "The Northeast Home Heating Oil Reserve," dated March 8, 2001. B- 5 Exemption -

287

The effect of highly structured cosmic magnetic fields on ultra-high energy cosmic ray propagation  

E-Print Network (OSTI)

The possibility that the magnetic field is strongly correlated with the large-scale structure of the universe has been recently considered in the literature. In this scenario the intergalactic magnetic field has a strong ($\\mu$G) regular component spanning tens of Mpc but localized in sheets and filaments, while the vast voids in between are almost free of magnetic field. If true, this could have important consequences on the propagation of ultra-high energy cosmic rays, and severely affect our capacity of doing astronomy with charged particles. A quantitative discussion of these effects is given in the present work.

Gustavo Medina Tanco

1998-08-07T23:59:59.000Z

288

The Kurtosis of the Cosmic Shear Field  

E-Print Network (OSTI)

We study the fourth-order moment of the cosmic shear field using the dark matter halo approach to describe the nonlinear gravitational evolution of structure in the universe. Since the third-order moment of the shear field vanishes because of symmetry, non-Gaussian signatures in its one-point statistics emerge at the fourth-order level. We argue that the shear kurtosis parameter S_4 = /^3 may be more directly applicable to realistic data than the well-studied higher-order statistics of the convergence field, since obtaining the convergence requires a non-local reconstruction from the measured shear field. We compare our halo model predictions for the variance, skewness and kurtosis of lensing fields with ray-tracing simulations of cold dark matter models and find good agreement. The shear kurtosis calculation is made tractable by developing approximations for fast and accurate evaluations of the 8-dimensional integrals needed to obtain the kurtosis. We show that on small scales it is dominated by correlations within halos more massive than 10^14 solar masses. The shear kurtosis is sensitive to the mass density parameter of the universe, Omega, and has relatively weak dependences on other parameters. The approximations we develop for the third- and fourth-order moments allow for accurate halo model predictions for the 3-dimensional mass distribution as well. We demonstrate their accuracy in the small scale regime, below 2 Mpc, where analytical approaches used in the literature so far cease to be accurate.

Masahiro Takada; Bhuvnesh Jain

2002-05-05T23:59:59.000Z

289

Cosmic Ray Spectrum in Supernova Remnant Shocks  

E-Print Network (OSTI)

We perform kinetic simulations of diffusive shock acceleration (DSA) in Type Ia supernova remnants (SNRs) expanding into a uniform interstellar medium (ISM). Bohm-like diffusion assumed, and simple models for Alfvenic drift and dissipation are adopted. Phenomenological models for thermal leakage injection are considered as well. We find that the preshock gas temperature is the primary parameter that governs the cosmic ray (CR) acceleration efficiency and energy spectrum, while the CR injection rate is a secondary parameter. For SNRs in the warm ISM, if the injection fraction is larger than 10^{-4}, the DSA is efficient enough to convert more than 20 % of the SN explosion energy into CRs and the accelerated CR spectrum exhibits a concave curvature flattening to E^{-1.6}. Such a flat source spectrum near the knee energy, however, may not be reconciled with the CR spectrum observed at Earth. On the other hand, SNRs in the hot ISM, with an injection fraction smaller than 10^{-4}, are inefficient accelerators with...

Kang, Hyesung

2010-01-01T23:59:59.000Z

290

A Cosmic Ray Telescope For Educational Purposes  

SciTech Connect

Cosmic ray detectors are widely used, for educational purposes, in order to motivate students to the physics of elementary particles and astrophysics. Using a 'telescope' of scintillation counters, the directional characteristics, diurnal variation, correlation with solar activity, can be determined, and conclusions about the composition, origin and interaction of elementary particles with the magnetic field of earth can be inferred. A telescope was built from two rectangular scintillator panels with dimensions: 91.6x1.9x3.7 cm{sup 3}. The scintillators are placed on top of each other, separated by a fixed distance of 34.6 cm. They are supported by a wooden frame which can be rotated around a horizontal axis. Direction is determined by the coincidence of the signals of the two PMTs. Standard NIM modules are used for readout. This device is to be used in the undergraduate nuclear and particle physics laboratory. The design and construction of the telescope as well as some preliminary results are presented.

Voulgaris, G.; Kazanas, S.; Chamilothoris, I. [Department of Physics, National and Kapodistrian University of Athens (Greece)

2010-01-21T23:59:59.000Z

291

Cosmic microwave background constraints on dark energy dynamics: analysis beyond the power spectrum  

E-Print Network (OSTI)

We consider the distribution of the non-Gaussian signal induced by weak lensing on the primary total intensity cosmic microwave background (CMB) anisotropies. Our study focuses on the three point statistics exploiting an harmonic analysis based on the CMB bispectrum. By considering the three multipoles as independent variables, we reveal a complex structure of peaks and valleys determined by the re-projection of the primordial acoustic oscillations through the lensing mechanism. We study the dependence of this system on the expansion rate at the epoch in which the weak lensing power injection is relevant, probing the dark energy equation of state at redshift corresponding to the equivalence with matter or higher ($w_\\infty$). We evaluate the impact of the bispectrum observable on the CMB capability of constraining the dark energy dynamics. We perform a maximum likelihood analysis by varying the dark energy abundance, the present equation of state $w_0$ and $w_\\infty$. We show that the projection degeneracy affecting a pure power spectrum analysis in total intensity is broken if the bispectrum is taken into account. For a Planck-like experiment, assuming nominal performance, no foregrounds or systematics, and fixing all the parameters except $w_0$, $w_\\infty$ and the dark energy abundance, a percent and ten percent precision measure of $w_0$ and $w_\\infty$ is achievable from CMB data only. These results indicate that the detection of the weak lensing signal by the forthcoming CMB probes may be relevant to gain insight into the dark energy dynamics at the onset of cosmic acceleration.

Fabio Giovi; Carlo Baccigalupi; Francesca Perrotta

2004-11-25T23:59:59.000Z

292

Energy Frontier Research Centers 2011 Summit and Forum: Science for our Nation's Energy Future (Videoed Presentations)  

DOE Data Explorer (OSTI)

Science for our NationÆs Energy Future, the 2011 Summit and Forum for and by DOEÆs Energy Frontier Research Centers (EFRC) was held May 2011 in Washington D.C. The videoed presentations are listed below. In addition, the same website provides access to the 26 videos created and submitted by some of the EFRCÆs as entries to the ôLife at the Frontiers of Energy Researchö research.

  • Welcome Remarks and Introduction from the DOE Under Secretary for Science, Steve Koonin
  • Energy Frontier Research Centers: Helping Win the Energy Innovation Race (2011 EFRC Summit Keynote Address, Secretary of Energy Chu)
  • Remarks from Congressional Leaders: Senator Jeff Bingaman
  • Remarks from Congressional Leaders: Congressman Daniel Lipinski
  • Remarks from Congressional Leaders: Congresswoman Zoe Lofgren
  • Introduction to the Summit Session, "Leading Perspectives in Energy Research", from the Director of the DOE Office of Science, Bill Brinkman
  • The Role of Research Universities in Helping Solve our Energy Challenges: A Case Study at Stanford and SLAC (John Hennessy)
  • Innovating a Sustainable Energy Future (Mark Little)
  • Perspectives in Energy Research: How Can We Change the Game? (Eric Isaccs)
  • Joint Center for Artificial Photosynthesis (JCAP): DOE's Solar Fuels Energy Innovation Hub (Nate Lewis)
  • Energy Frontier Research Centers (EFRCs): A Response to Five Challenges for Science and the Imagination (panel session)
  • Science for Energy Technology: The Industry Perspective (panel session)
  • Energy Frontier Research Centers: A View from Senior EFRC Representatives (panel session)
  • Facing Our Energy Challenges in a New Era of Science (Pat Dehmer, Forum Session)
  • Basic Solar Energy Research in Japan (Kazunari Domen, Forum Session)
  • A Resurgence of United Kingdom Nuclear Power Research (Robin Grimes, Forum Session)
  • Key Challenges and New Trends in Battery Research (Jean Marie Tarascon, Forum Session)

293

Measuring the energy efficiency of households: an application of frontier production function analysis  

SciTech Connect

A new method to estimate the energy efficiency of households is presented. Households are viewed as productive units organized to provide the occupants with numerous services requiring fuel as an input: house heating to achieve a desired interior temperature, lighting for recreation, etc. The focus is on the efficiency of energy use, not the demand for energy. The approach to measuring efficiency compares a group of productive units along several dimensions of input resources and service outputs. The comparison identifies a subset of units that are considered efficient because they require the least resources per unit of service provided. The efficient units form a production possibility frontier of best practice in service provision. A regression of the two sets of efficiency scores on other variables reflecting locational, dwelling unit, and occupational characteristics is performed to identify factors accounting for differences in efficiency. The results indicate that the more efficient units used electric heat, had higher ratios of non-electric to electric fuel inputs, were owner-occupied, and were built after 1974. The findings also suggest that both family life cycle and income effects account for efficiency differences.

Baxter, L.W.

1984-01-01T23:59:59.000Z

294

Electron Ion Collider: The Next QCD Frontier - Understanding the glue that binds us all  

E-Print Network (OSTI)

This White Paper presents the science case of an Electron-Ion Collider (EIC), focused on the structure and interactions of gluon-dominated matter, with the intent to articulate it to the broader nuclear science community. It was commissioned by the managements of Brookhaven National Laboratory (BNL) and Thomas Jefferson National Accelerator Facility (JLab) with the objective of presenting a summary of scientific opportunities and goals of the EIC as a follow-up to the 2007 NSAC Long Range plan. This document is a culmination of a community-wide effort in nuclear science following a series of workshops on EIC physics and, in particular, the focused ten-week program on "Gluons and quark sea at high energies" at the Institute for Nuclear Theory in Fall 2010. It contains a brief description of a few golden physics measurements along with accelerator and detector concepts required to achieve them, and it benefited from inputs from the users' communities of BNL and JLab. This White Paper offers the promise to propel the QCD science program in the U.S., established with the CEBAF accelerator at JLab and the RHIC collider at BNL, to the next QCD frontier.

A. Accardi; J. L. Albacete; M. Anselmino; N. Armesto; E. C. Aschenauer; A. Bacchetta; D. Boer; W. Brooks; T. Burton; N. -B. Chang; W. -T. Deng; A. Deshpande; M. Diehl; A. Dumitru; R. Dupré; R. Ent; S. Fazio; H. Gao; V. Guzey; H. Hakobyan; Y. Hao; D. Hasch; R. Holt; T. Horn; M. Huang; A. Hutton; C. Hyde; J. Jalilian-Marian; S. Klein; B. Kopeliovich; Y. Kovchegov; K. Kumar; K. Kumeri?ki; M. A. C. Lamont; T. Lappi; J. -H. Lee; Y. Lee; E. M. Levin; F. -L. Lin; V. Litvinenko; T. W. Ludlam; C. Marquet; Z. -E. Meziani; R. McKeown; A. Metz; R. Milner; V. S. Morozov; A. H. Mueller; B. Müller; D. Müller; P. Nadel-Turonski; A. Prokudin; V. Ptitsyn; X. Qian; J. -W. Qiu; M. Ramsey-Musolf; T. Roser; F. Sabatié; R. Sassot; G. Schnell; P. Schweitzer; E. Sichtermann; M. Stratmann; M. Strikman; M. Sullivan; S. Taneja; T. Toll; D. Trbojevic; T. Ullrich; R. Venugopalan; S. Vigdor; W. Vogelsang; C. Weiss; B. -W. Xiao; F. Yuan; Y. -H. Zhang; L. Zheng

2012-12-07T23:59:59.000Z

295

ITP Energy Intensive Processes: Energy-Intensive Processes Portfolio...  

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

for energy-Intensive Processes (eIP) addresses the top technology opportunities to save energy and reduce carbon emissions across the industrial sector. the portfolio focuses the...

296

Feedback Heating by Cosmic Rays in Clusters of Galaxies  

E-Print Network (OSTI)

Recent observations show that the cooling flows in the central regions of galaxy clusters are highly suppressed. Observed AGN-induced cavities/bubbles are a leading candidate for suppressing cooling, usually via some form of mechanical heating. At the same time, observed X-ray cavities and synchrotron emission point toward a significant non-thermal particle population. Previous studies have focused on the dynamical effects of cosmic-ray pressure support, but none have built successful models in which cosmic-ray heating is significant. Here we investigate a new model of AGN heating, in which the intracluster medium is efficiently heated by cosmic-rays, which are injected into the ICM through diffusion or the shredding of the bubbles by Rayleigh-Taylor or Kelvin-Helmholtz instabilities. We include thermal conduction as well. Using numerical simulations, we show that the cooling catastrophe is efficiently suppressed. The cluster quickly relaxes to a quasi-equilibrium state with a highly reduced accretion rate and temperature and density profiles which match observations. Unlike the conduction-only case, no fine-tuning of the Spitzer conduction suppression factor f is needed. The cosmic ray pressure, P_c/P_g alternative to mechanical heating, and may become particularly compelling if GLAST detects the gamma-ray signature of cosmic-rays in clusters.

Fulai Guo; S. Peng OH

2007-06-09T23:59:59.000Z

297

Reference Radiation for Cosmic Rays in RBE Research  

E-Print Network (OSTI)

When astronauts travel in space, they are exposed to high energy cosmic radiations. The cosmic ray spectrum contains very high energy particles, generally up to several GeV per nucleon. Currently NASA is funding research on the effects, such as acute radiation sickness, of cosmic radiation. Animal models are used to conduct the studies of radiation effects of particles in the range of several MeV/nucleon to about 1000 MeV/nucleon. In order to compare different radiations, the biological effectiveness relative to a specific radiation is usually used. For low energy heavy ions and neutrons 250 keV photons are usually used for the reference radiation but their depth dose distribution is very different from that for cosmic rays. In this research, the advantages of using high energy electrons as the reference radiation for research on cosmic radiation were demonstrated. The conclusion is based on the evaluation of the dose distributions and microdosimetric spectra of the electrons and high energy protons as a function of depth in a tissue equivalent absorber as determined by Geant4 simulation.

Feng, Shaoyong

2010-08-01T23:59:59.000Z

298

energy intensity | OpenEI  

Open Energy Info (EERE)

intensity intensity Dataset Summary Description Energy intensity data and documentation published by the U.S. DOE's office of Energy Efficiency and Renewable Energy (EERE). Energy intensity is defined as: amount of energy used in producing a given level of output or activity; expressed as energy per unit of output. This is the energy intensity of the the electricity sector, which is an energy consuming sector that generates electricity. Data are organized to separate electricity-only generators from combined heat and power (CHP) generators. Data is available for the period 1949 - 2004. Source EERE Date Released May 31st, 2006 (8 years ago) Date Updated Unknown Keywords Electricity Energy Consumption energy intensity fossil fuels renewable energy Data application/vnd.ms-excel icon electricity_indicators.xls (xls, 2.1 MiB)

299

The Cosmic Ray Muon Flux at WIPP  

E-Print Network (OSTI)

In this work a measurement of the muon intensity at the Waste Isolation Pilot Plant (WIPP) near Carlsbad, NM, USA is presented. WIPP is a salt mine with a depth of 655 m. The vertical muon flux was measured with a two panels scintillator coincidence setup to Phi_{vert}=3.10(+0.05/-0.07)*10^(-7)s^(-1)cm^(-2)sr^(-1).

E. -I. Esch; T. J. Bowles; A. Hime; A. Pichlmaier; R. Reifarth; H. Wollnik

2004-08-25T23:59:59.000Z

300

The Cosmic Ray Muon Flux at WIPP  

E-Print Network (OSTI)

In this work a measurement of the muon intensity at the Waste Isolation Pilot Plant (WIPP) near Carlsbad, NM, USA is presented. WIPP is a salt mine with a depth of 655 m. The vertical muon flux was measured with a two panels scintillator coincidence setup to ?vert = (3.10 +0.05 ?0.07) 10?7 s ?1 cm ?2 sr ?1.

E. -i. Esch A; T. J. Bowles A; A. Hime A; A. Pichlmaier A; R. Reifarth A; H. Wollnik B

2004-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


301

The Cosmic Ray Muon Flux at WIPP  

E-Print Network (OSTI)

In this work a measurement of the muon intensity at the Waste Isolation Pilot Plant (WIPP) near Carlsbad, NM, USA is presented. WIPP is a salt mine with a depth of 655 m. The vertical muon flux was measured with a two panels scintillator coincidence setup to Phi_{vert}=3.10(+0.05/-0.07)*10^(-7)s^(-1)cm^(-2)sr^(-1).

Esch, E I; Hime, A; Pichlmaier, A; Reifarth, R; Wollnik, H

2005-01-01T23:59:59.000Z

302

Investigating Possible Links between Incoming Cosmic Ray Fluxes and Lightning Activity over the United States  

Science Conference Proceedings (OSTI)

During the past two decades, particular scientific attention has been drawn to the potential cosmic ray–atmospheric coupling. Galactic cosmic rays reaching the upper troposphere are suggested as the key modulators of the global electric circuit, ...

Themis G. Chronis

2009-11-01T23:59:59.000Z

303

Cosmic-ray Propagation and Interactions in the Galaxy  

Science Conference Proceedings (OSTI)

We survey the theory and experimental tests for the propagation of cosmic rays in the Galaxy up to energies of 10{sup 15} eV. A guide to the previous reviews and essential literature is given, followed by an exposition of basic principles. The basic ideas of cosmic-ray propagation are described, and the physical origin of its processes are explained. The various techniques for computing the observational consequences of the theory are described and contrasted. These include analytical and numerical techniques. We present the comparison of models with data including direct and indirect--especially gamma-ray--observations, and indicate what we can learn about cosmic-ray propagation. Some particular important topics including electrons and antiparticles are chosen for discussion.

Strong, Andrew W.; /Garching, Max Planck Inst., MPE; Moskalenko, Igor V.; /Stanford U., HEPL /KIPAC, Menlo Park; Ptuskin, Vladimir S.; /Troitsk, IZMIRAN

2007-01-22T23:59:59.000Z

304

Quantum Indeterminacy in Local Measurement of Cosmic Expansion  

E-Print Network (OSTI)

For a system of two small bodies in an expanding universe, bounds on mass and separation are estimated, from standard gravity and quantum mechanics, such that both their gravity and the process of quantum measurement affect their motion less than the cosmic expansion does. It is shown that such a direct local measurement of cosmic expansion or acceleration at rate $H$ is only possible, even in principle, in a region of size greater than $H^{-3/5}$ in Planck units, or about 60 meters in the current universe, a new scale that defines a boundary between quantum and classical expansion. A generalization to spatially extended linear density perturbations shows the same scale. Matching vacuum energy or directional information in localized field states to gravity on this system length scale yields a particle mass scale of $H^{3/10}$, or about 7 GeV today. Possible connections of cosmic acceleration with the QCD vacuum are discussed.

Craig J. Hogan

2013-12-30T23:59:59.000Z

305

Quantum indeterminacy in local measurement of cosmic expansion  

E-Print Network (OSTI)

For a system of two small bodies in an expanding universe, bounds on mass and separation are estimated, from standard gravity and quantum mechanics, such that both their gravity and the process of quantum measurement affect their motion less than the cosmic expansion does. It is shown that such a direct local measurement of cosmic expansion or acceleration at rate $H$ is only possible, even in principle, in a region of size greater than $H^{-3/5}$ in Planck units, or about 60 meters in the current universe, a new scale that defines a boundary between quantum and classical expansion. A generalization to spatially extended linear density perturbations shows the same scale. Matching vacuum energy or directional information in localized field states to gravity on this system length scale yields a particle mass scale of $H^{3/10}$, or about 7 GeV today. Possible connections of cosmic acceleration with the QCD vacuum are discussed.

Hogan, Craig J

2013-01-01T23:59:59.000Z

306

Tests for Gaussianity of the MAXIMA-1 cosmic microwave backgroundmap  

SciTech Connect

Gaussianity of the cosmological perturbations is one of the key predictions of standard inflation, but it is violated by other models of structure formation such as cosmic defects. We present the first test of the Gaussianity of the cosmic microwave background (CMB) on subdegree angular scales, where deviations from Gaussianity are most likely to occur. We apply the methods of moments, cumulants, the Kolmogorov test, the chi (2) test, and Minkowski functionals in eigen, real, Wiener-filtered, and signal-whitened spaces, to the MAXIMA-1 CMB anisotropy data. We find that the data, which probe angular scales between 10 arcmin and 5 deg, are consistent with Gaussianity. These results show consistency with the standard inflation and place constraints on the existence of cosmic defects.

Wu, J.H.P.; Balbi, A.; Borrill, J.; Ferreira, P.G.; Hanany, S.; Jaffe, A.H.; Lee, A.T.; Rabii, B.; Richards, P.L.; Smoot, G.F.; Stompor,R.; Winant, C.D.

2001-04-14T23:59:59.000Z

307

Cosmic parallax as a probe of late time anisotropic expansion  

SciTech Connect

Cosmic parallax is the change of angular separation between a pair of sources at cosmological distances induced by an anisotropic expansion. An accurate astrometric experiment like Gaia could observe or put constraints on cosmic parallax. Examples of anisotropic cosmological models are Lemaitre-Tolman-Bondi void models for off-center observers (introduced to explain the observed acceleration without the need for dark energy) and Bianchi metrics. If dark energy has an anisotropic equation of state, as suggested recently, then a substantial anisotropy could arise at z < or approx. 1 and escape the stringent constraints from the cosmic microwave background. In this paper we show that such models could be constrained by the Gaia satellite or by an upgraded future mission.

Quercellini, Claudia; Cabella, Paolo; Balbi, Amedeo [Universita di Roma Tor Vergata, Via della Ricerca Scientifica 1, 00133 Roma (Italy); Amendola, Luca [INAF/Osservatorio Astronomico di Roma, V. Frascati 33, 00040 Monteporzio Catone, Roma (Italy); Quartin, Miguel [INAF/Osservatorio Astronomico di Roma, V. Frascati 33, 00040 Monteporzio Catone, Roma (Italy); Institut fuer Theoretische Physik, Universitaet Heidelberg, Philosophenweg 16, 69120 Heidelberg (Germany)

2009-09-15T23:59:59.000Z

308

Search for Cosmic Strings in the GOODS Survey  

E-Print Network (OSTI)

We search Hubble Space Telescope Treasury Program images collected as part of the Great Observatories Origins Deep Survey for pairs of galaxies consistent with the gravitational lensing signature of a cosmic string. Our technique includes estimates of the efficiency for finding the lensed galaxy pair. In the north (south) survey field we find no evidence out to a redshift of greater than 0.5 (0.3) for cosmic strings to a mass per unit length limit of $G\\musearches for individual strings in cosmic microwave background (CMB) data. Our limit is higher than other CMB and gravitational wave searches, however, we note that it is less model dependent than these other searches.

J. L. Christiansen; E. Albin; K. A. James; J. Goldman; D. Maruyama; G. F. Smoot

2008-02-29T23:59:59.000Z

309

A study of the link between cosmic rays and clouds with a cloud chamber at the CERN PS  

E-Print Network (OSTI)

Recent satellite data have revealed a surprising correlation between galactic cosmic ray (GCR) intensity and the fraction of the Earth covered by clouds. If this correlation were to be established by a causal mechanism, it could provide a crucial step in understanding the long-sought mechanism connecting solar and climate variability. The Earth's climate seems to be remarkably sensitive to solar activity, but variations of the Sun's electromagnetic radiation appear to be too small to account for the observed climate variability. However, since the GCR intensity is strongly modulated by the solar wind, a GCR-cloud link may provide a sufficient amplifying mechanism. Moreover if this connection were to be confirmed, it could have profound consequences for our understanding of the solar contributions to the current global warming. The CLOUD (Cosmics Leaving OUtdoor Droplets) project proposes to test experimentally the existence a link between cosmic rays and cloud formation, and to understand the microphysical mechanism. CLOUD plans to perform detailed laboratory measurements in a particle beam at CERN, where all the parameters can be precisely controlled and measured. The beam will pass through an expansion cloud chamber and a reactor chamber where the atmosphere is to be duplicated by moist air charged with selected aerosols and trace condensable vapours. An array of external detectors and mass spectrometers is used to analyse the physical and chemical characteristics of the aerosols and trace gases during beam exposure. Where beam effects are found, the experiment will seek to evaluate their significance in the atmosphere by incorporating them into aerosol and cloud models.

The Cloud Collaboration

2001-04-16T23:59:59.000Z

310

Gamma-Ray Bursts, Ultra High Energy Cosmic Rays, and Cosmic Gamma-Ray Background  

E-Print Network (OSTI)

We argue that gamma-ray bursts (GRBs) may be the origin of the cosmic gamma-ray background radiation observed in GeV range. It has theoretically been discussed that protons may carry a much larger amount of energy than electrons in GRBs, and this large energy can be radiated in TeV range by synchrotron radiation of ultra-high-energy protons (\\sim 10^{20} eV). The possible detection of GRBs above 10 TeV suggested by the Tibet and HEGRA groups also supports this idea. If this is the case, most of TeV gamma-rays from GRBs are absorbed in intergalactic fields and eventually form GeV gamma-ray background, whose flux is in good agreement with the recent observation.

Tomonori Totani

1998-10-14T23:59:59.000Z

311

Passive Imaging of Warhead-Like Configurations Using Cosmic-Ray Muons  

SciTech Connect

Cosmic-Muon-Based Interrogation has untapped potential for national security. This presentation describes muons-based passive interrogation techniques.

Schwellenbach, D.

2012-07-17T23:59:59.000Z

312

THE RELATION BETWEEN POST-SHOCK TEMPERATURE, COSMIC-RAY PRESSURE, AND COSMIC-RAY ESCAPE FOR NON-RELATIVISTIC SHOCKS  

Science Conference Proceedings (OSTI)

Supernova remnants (SNRs) are thought to be the dominant source of Galactic cosmic rays. This requires that at least 5% of the available energy is transferred to cosmic rays, implying a high cosmic-ray pressure downstream of SNR shocks. Recently, it has been shown that the downstream temperature in some remnants is low compared to the measured shock velocities, implying that additional pressure supported by accelerated particles is present. Here we use a two-fluid thermodynamic approach to derive the relation between post-shock fractional cosmic-ray pressure and post-shock temperature, assuming no additional heating beyond adiabatic heating in the shock precursor and with all non-adiabatic heating occurring at the subshock. The derived relations show that a high fractional cosmic-ray pressure is only possible if a substantial fraction of the incoming energy flux escapes from the system. Recently, a shock velocity and a downstream proton temperature were measured for a shock in the SNR RCW 86. We apply the two-fluid solutions to these measurements and find that the downstream fractional cosmic-ray pressure is at least 50% with a cosmic-ray energy flux escape of at least 20%. In general, in order to have 5% of the supernova energy to go into accelerating cosmic rays, on average the post-shock cosmic-ray pressure needs to be 30% for an effective cosmic-ray adiabatic index of {gamma}{sub cr} = 4/3.

Vink, Jacco; Helder, Eveline A.; Schure, K. M. [Astronomical Institute, Utrecht University, P.O. Box 80000, 3508 TA Utrecht (Netherlands); Yamazaki, Ryo, E-mail: j.vink@astro-uu.n [Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara, Kanagawa 252-5258 (Japan)

2010-10-20T23:59:59.000Z

313

Cosmic Ray Sun Shadow in Soudan 2 Underground Muon Flux  

E-Print Network (OSTI)

The absorption of cosmic rays by the sun produces a shadow at the earth. The angular offset and broadening of the shadow are determined by the magnitude and structure of the interplanetary magnetic field (IPMF) in the inner solar system. We report the first measurement of the solar cosmic ray shadow by detection of deep underground muon flux in observations made during the entire ten-year interval 1989 to 1998. The sun shadow varies significantly during this time, with a $3.3\\sigma$ shadow observed during the years 1995 to 1998.

Soudan 2 Collaboration

1999-05-24T23:59:59.000Z

314

Imprint of Sterile Neutrinos in the Cosmic Microwave Background Radiation  

E-Print Network (OSTI)

The existence of low-mass sterile neutrinos is suggested by the current status of solar and atmospheric neutrinos together with the LSND experiment. In typical four-flavor scenarios, neutrinos would contribute to a cosmic hot dark matter component and to an increased radiation content at the epoch of matter-radiation equality. These effects leave their imprint in sky maps of the cosmic microwave background radiation (CMBR) and may thus be detectable with the precision measurements of the upcoming MAP and PLANCK missions.

Steen Hannestad; Georg Raffelt

1998-05-17T23:59:59.000Z

315

Energy spectrum of ultra high energy cosmic rays  

E-Print Network (OSTI)

The construction of the southern site of the Pierre Auger Observatory is almost completed. Three independent measurements of the flux of the cosmic rays with energies larger than 1 EeV have been performed during the construction phase. The surface detector data collected until August 2007 have been used to establish a flux suppression at the highest energies with a 6 sigma significance. The observations of cosmic rays by the fluorescence detector allowed the extension of the energy spectrum to lower energies, where the efficiency of the surface detector is less than 100% and a change in the spectral index is expected.

Ioana C. Maris; for the Pierre Auger Collaboration

2008-08-12T23:59:59.000Z

316

Phenomenology of Multi-W Processes in Cosmic Rays  

E-Print Network (OSTI)

We report on a study of the potential of various cosmic ray physics experiments to search for Standard Model processes involving the nonperturbative production of O(30) weak gauge bosons. Whereas present and near-future experiments are insensitive to proton-induced processes, neutrino-induced processes give rise to promising signatures and rates in AMANDA, DUMAND, MACRO and NESTOR provided that a cosmic neutrino flux exists at levels suggested by recent models of active galactic nuclei. The Fly's Eye currently constrains the largest region of parameter space characterizing multi-W phenomena.

D. A. Morris; A. Ringwald

1993-09-14T23:59:59.000Z

317

Cosmic Ray Signatures of Multi-W Processes  

E-Print Network (OSTI)

We explore the discovery potential of cosmic ray physics experiments for Standard Model processes involving the nonperturbative production of O(30) weak gauge bosons. We demonstrate an experimental insensitivity to proton-induced processes and emphasize the importance of neutrino-induced processes. The Fly's Eye currently constrains the largest region of parameter space characterizing multi-W phenomena if a cosmic neutrino flux exists at levels suggested by recent models of active galactic nuclei. MACRO (DUMAND) can constrain or observe additional regions by searching for 1-100 (1-10) characteristic near-vertical (near-horizontal) spatially compact energetic muon bundles per year.

D. A. Morris; A. Ringwald

1993-08-13T23:59:59.000Z

318

Calibrating laser test-beams for cosmic-ray observatories  

E-Print Network (OSTI)

Pulsed UV lasers can provide useful "testbeams" for observatories that use optical detectors, especially fluorescence detectors, to measure high energy cosmic-rays. The light observed by the detector is proportional to the energy of the laser pulse. Since the absolute laser energy can be measured locally, a well-calibrated laser offers a practical way to test the photometric calibration of the cosmic-ray detector including atmospheric corrections. This poster will describe a robotic system for laser polarization and energy calibration. Laboratory measurements of laser energies and polarizations by energy probes from different manufactures will be presented

Wiencke, Lawrence; Compton, John; Monasor, Maria; Pilger, David; Rosado, Jaime

2011-01-01T23:59:59.000Z

319

CMS Data Processing Workflows during an Extended Cosmic Ray Run  

Science Conference Proceedings (OSTI)

The CMS Collaboration conducted a month-long data taking exercise, the Cosmic Run At Four Tesla, during October-November 2008, with the goal of commissioning the experiment for extended operation. With all installed detector systems participating, CMS recorded 270 million cosmic ray events with the solenoid at a magnetic field strength of 3.8 T. This paper describes the data flow from the detector through the various online and offline computing systems, as well as the workflows used for recording the data, for aligning and calibrating the detector, and for analysis of the data.

Not Available

2009-11-01T23:59:59.000Z

320

Similarities and Distinctions in Cosmic-Ray Modulation during Different Phases of Solar and Magnetic Activity Cycles  

E-Print Network (OSTI)

We study the solar-activity and solar-polarity dependence of galactic cosmic-ray intensity (CRI) on the solar and heliospheric parameters playing a significant role in solar modulation. We utilize the data for cosmic-ray intensity as measured by neutron monitors, solar activity as measured by sunspot number (SSN), interplanetary plasma/field parameters, solar-wind velocity [V] and magnetic field [B], as well as the tilt of the heliospheric current sheet [{\\Lambda}] and analyse these data for Solar Cycles 20 - 24 (1965 - 2011). We divide individual Solar Cycles into four phases, i.e. low, high, increasing, and decreasing solar activity. We perform regression analysis to calculate and compare the CRI-response to changes in different solar/interplanetary parameters during (i) different phases of solar activity and (ii) similar activity phases but different polarity states. We find that the CRI-response is different during negative (A0) polarity states not only with SSN and {\\Lambda} but also with B and V. The re...

Aslam, O P M

2013-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
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321

Mapping of the cosmic ray events related to the solar activity for the period 2003-2005  

E-Print Network (OSTI)

The relationship between cosmic ray intensity decreases and solar events is still an open field of space research. In this work a complete study of solar events occurred from January 2003 to December 2005, is considered. This three-years time period characterized by an unexpected activity of the Sun was divided into 27-day intervals starting from BR 2313 (06.01.2003) to 2353 (21.12.2005), generating diagrams of the cosmic ray intensity data recorded at the Athens Neutron Monitor Station. This station is working at an altitude of 260m and cut-off rigidity 8.53GV provided to the Internet high-resolution data in real-time. A mapping of all available solar and interplanetary events, such as solar flares with importance M and X, coronal mass ejections (Halo and Partial) was done. As we are going down from the solar maximum to the declining phase of the 23rd solar cycle, a statistical overview of the corresponding relationship among these phenomena, the significant percentage of the connection of Halo CMEs and sola...

Papaioannou, A; Mavromichalaki, H

2010-01-01T23:59:59.000Z

322

Detection of the Cosmic Infrared Background at 2.2 and 3.5 microns Using DIRBE Observations  

E-Print Network (OSTI)

We compare data from the Diffuse InfraRed Background Experiment (DIRBE) on the Cosmic Background Explorer (COBE) satellite to the the Wainscoat et al. (1992) model of the infrared sky. The model is first compared with broadband K (2.2 microns) star counts. Its success at K gives credence to its physical approach which is extrapolated to the L band (3.5 microns). We have analyzed the histograms of the pixel by pixel intensities in the 2.2 and 3.5 micron maps from DIRBE after subtracting the zodiacal light. The shape of these histograms agrees quite well with the histogram shape predicted using the Wainscoat et al. model of the infrared sky, but the predicted histograms must be displaced by a constant intensity in order to match the data. This shift is the cosmic infrared background, which is 16.9+/-4.4 kJy/sr or 23.1+/-5.9 nW/m^2/sr at 2.2 microns, and 14.4+/-3.7 kJy/sr or 12.4+/-3.2 nW/m^2/sr at 3.5 microns.

E. L. Wright; E. D. Reese

1999-12-27T23:59:59.000Z

323

The Fluid Interface Reactions Structures and Transport (FIRST) EFRC (A "Life at the Frontiers of Energy Research" contest entry from the 2011 Energy Frontier Research Centers (EFRCs) Summit and Forum)  

DOE Green Energy (OSTI)

'The Fluid Interface Reactions Structures and Transport (FIRST) EFRC' was submitted by FIRST to the 'Life at the Frontiers of Energy Research' video contest at the 2011 Science for Our Nation's Energy Future: Energy Frontier Research Centers (EFRCs) Summit and Forum. Twenty-six EFRCs created short videos to highlight their mission and their work. FIRST, an EFRC directed by David J. Wesolowski at the Oak Ridge National Laboratory is a partnership of scientists from nine institutions: Oak Ridge National Laboratory (lead), Argonne National Laboratory, Drexel University, Georgia State University, Northwestern University, Pennsylvania State University, Suffolk University, Vanderbilt University, and University of Virginia. The Office of Basic Energy Sciences in the U.S. Department of Energy's Office of Science established the 46 Energy Frontier Research Centers (EFRCs) in 2009. These collaboratively-organized centers conduct fundamental research focused on 'grand challenges' and use-inspired 'basic research needs' recently identified in major strategic planning efforts by the scientific community. The overall purpose is to accelerate scientific progress toward meeting the nation's critical energy challenges. The mission of Fluid Interface Reactions, Structures and Transport Center is 'to develop quantitative and predictive models of the unique nanoscale environment at fluid-solid interfaces that will enable transformational advances in electrical energy storage and heterogeneous catalysis for solar fuels.' Research topics are: catalysis (biomass, CO{sub 2}, water), electrocatalysis, photocatalysis, photoelectrocatalysis, solar fuels, solar electrodes, electrical energy storage, batteries, capacitors, battery electrodes, electrolytes, extreme environment, CO{sub 2} (convert), greenhouse gas, microelectromechanical systems (MEMS), interfacial characterization, matter by design, novel materials synthesis, and charge transport.

Wesolowski, David J. (Director, FIRST - Fluid Interface Reactions, Structures, and Transport Center); FIRST Staff

2011-05-01T23:59:59.000Z

324

Frontiers in Microbiology: Envisioning a Curriculum Unit for High School Biology  

Science Conference Proceedings (OSTI)

Microbiology is undergoing a quiet revolution. Techniques such as polymerase chain reaction, high throughput DNA sequencing, whole genome shotgun sequencing, DNA microarrays, and bioinformatics analyses are greatly aiding our understanding of the estimated one billion species of microbes that inhabit the Earth. Unfortunately, the rapid pace of research in microbiology stands in contrast to the much slower pace of change in educational reform. Biological Sciences Curriculum Study (BSCS) hosted a two-day planning meeting to discuss whether or not a new curriculum unit on microbiology is desirable for the high school audience. Attending the meeting were microbiologists, high school biology teachers, and science educators. The consensus of the participants was that an inquiry-based unit dealing with advances in microbiology should be developed for a high school biology audience. Participants established content priorities for the unit, discussed the unit's conceptual flow, brainstormed potential student activities, and discussed the role of educational technology for the unit. As a result of the planning meeting discussions, BSCS staff sought additional funding to develop, disseminate, and evaluate the Frontiers in Microbiology curriculum unit. This unit was intended to be developed as a replacement unit suitable for an introductory biology course. The unit would feature inquiry-based student activities and provide approximately four weeks of instruction. As appropriate, activities would make use of multimedia. The development and production processes would require about two years for completion. Unfortunately, BSCS staff was not able to attract sufficient funding to develop the proposed curriculum unit. Since there were some unexpended funds left over from the planning meeting, BSCS requested and received permission from DOE to use the balance of the funds to prepare background materials about advances in microbiology that would be useful to teachers. These materials were developed and placed on the BSCS Web site (http://www.bscs.org).

Mark Bloom

2004-06-18T23:59:59.000Z

325

Energy Frontier Research Centers: A View from Senior EFRC Representatives (2011 EFRC Summit, panel session)  

Science Conference Proceedings (OSTI)

A distinguished panel of scientists from the EFRC community provide their perspective on the importance of EFRCs for addressing critical energy needs at the 2011 EFRC Summit. Persis Drell, Director at SLAC, served as moderator. Panel members are Neal Armstrong (Director of the Center for Interface Science: Solar Electric Materials, led by the University of Arizona), Emily Carter (Co-Director of the Combustion EFRC, led by Princeton University. She is also Team Leader of the Heterogeneous Functional Materials Center, led by the University of South Caroline), Don DePaolo (Director of the Center for Nanoscale Control of Geologic CO2, led by LBNL), and Brent Gunnoe (Director of the Center for Catalytic Hydrocarbon Functionalization, led by the University of Virginia). The 2011 EFRC Summit and Forum brought together the EFRC community and science and policy leaders from universities, national laboratories, industry and government to discuss "Science for our Nation's Energy Future." In August 2009, the Office of Science established 46 Energy Frontier Research Centers. The EFRCs are collaborative research efforts intended to accelerate high-risk, high-reward fundamental research, the scientific basis for transformative energy technologies of the future. These Centers involve universities, national laboratories, nonprofit organizations, and for-profit firms, singly or in partnerships, selected by scientific peer review. They are funded at $2 to $5 million per year for a total planned DOE commitment of $777 million over the initial five-year award period, pending Congressional appropriations. These integrated, multi-investigator Centers are conducting fundamental research focusing on one or more of several “grand challenges” and use-inspired “basic research needs” recently identified in major strategic planning efforts by the scientific community. The purpose of the EFRCs is to integrate the talents and expertise of leading scientists in a setting designed to accelerate research that transforms the future of energy and the environment.

Drell, Persis (SLAC); Armstrong, Neal (University of Arizona); Carter, Emily (Princeton University); DePaolo, Don (Lawrence Berkeley National Laboratory); Gunnoe, Brent (University of Virginia)

2011-05-25T23:59:59.000Z

326

Energy Frontier Research Center, Center for Materials Science of Nuclear Fuels  

SciTech Connect

The Office of Science, Basic Energy Sciences, has funded the INL as one of the Energy Frontier Research Centers in the area of material science of nuclear fuels. This document is the required annual report to the Office of Science that outlines the accomplishments for the period of May 2010 through April 2011. The aim of the Center for Material Science of Nuclear Fuels (CMSNF) is to establish the foundation for predictive understanding of the effects of irradiation-induced defects on thermal transport in oxide nuclear fuels. The science driver of the center’s investigation is to understand how complex defect and microstructures affect phonon mediated thermal transport in UO2, and achieve this understanding for the particular case of irradiation-induced defects and microstructures. The center’s research thus includes modeling and measurement of thermal transport in oxide fuels with different levels of impurities, lattice disorder and irradiation-induced microstructure, as well as theoretical and experimental investigation of the evolution of disorder, stoichiometry and microstructure in nuclear fuel under irradiation. With the premise that thermal transport in irradiated UO2 is a phonon-mediated energy transport process in a crystalline material with defects and microstructure, a step-by-step approach will be utilized to understand the effects of types of defects and microstructures on the collective phonon dynamics in irradiated UO2. Our efforts under the thermal transport thrust involved both measurement of diffusive phonon transport (an approach that integrates over the entire phonon spectrum) and spectroscopic measurements of phonon attenuation/lifetime and phonon dispersion. Our distinct experimental efforts dovetail with our modeling effort involving atomistic simulation of phonon transport and prediction of lattice thermal conductivity using the Boltzmann transport framework.

Todd R. Allen, Director

2011-04-01T23:59:59.000Z

327

COBE Observations of the Cosmic Infrared Background  

E-Print Network (OSTI)

The Diffuse InfraRed Background Experiment on COBE measured the total infrared signal seen from space at a distance of 1 astronomical unit from the Sun. Using time variations as the Earth orbits the Sun, it is possible to remove most of the foreground signal produced by the interplanetary dust cloud [zodiacal light]. By correlating the DIRBE signal with the column density of atomic hydrogen measured using the 21 cm line, it is possible to remove most of the foreground signal produced by interstellar dust, although one must still be concerned by dust associated with H_2 (molecular gas) and H II (the warm ionized medium). DIRBE was not able to determine the CIRB in the 5-60 micron wavelength range, but did detect both a far infrared background and a near infrared background. The far infrared background has an integrated intensity of about 34 nW/m^2/sr, while the near infrared and optical extragalactic background has about 59 nW/m^2/sr. The Far InfraRed Absolute Spectrophotometer (FIRAS) on COBE has been used to constrain the long wavelength tail of the far infrared background but a wide range of intensities at 850 microns are compatible with the FIRAS data. Thus the fraction of the CIRB produced by SCUBA sources has large uncertainties in both the numerator and the denominator.

E. L. Wright

2003-06-03T23:59:59.000Z

328

QuarkNet/Walta/CROP Cosmic Ray Detectors  

E-Print Network (OSTI)

QuarkNet/Walta/CROP Cosmic Ray Detectors User's Manual Jeff Rylander and Tom Jordan, Fermilab R. J. Project Development Team Fermilab: Sten Hansen, Tom Jordan, Terry Kiper Univeristy of Nebraska: Dan Claes energies. However, it is possi- ble to do high-energy physics in your school without a particle accelerator

California at Santa Cruz, University of

329

DISCREPANT HARDENING OBSERVED IN COSMIC-RAY ELEMENTAL SPECTRA  

Science Conference Proceedings (OSTI)

The balloon-borne Cosmic Ray Energetics And Mass experiment launched five times from Antarctica has achieved a cumulative flight duration of about 156 days above 99.5% of the atmosphere. The instrument is configured with complementary and redundant particle detectors designed to extend direct measurements of cosmic-ray composition to the highest energies practical with balloon flights. All elements from protons to iron nuclei are separated with excellent charge resolution. Here, we report results from the first two flights of {approx}70 days, which indicate hardening of the elemental spectra above {approx}200 GeV/nucleon and a spectral difference between the two most abundant species, protons and helium nuclei. These results challenge the view that cosmic-ray spectra are simple power laws below the so-called knee at {approx}10{sup 15} eV. This discrepant hardening may result from a relatively nearby source, or it could represent spectral concavity caused by interactions of cosmic rays with the accelerating shock. Other possible explanations should also be investigated.

Ahn, H. S.; Ganel, O.; Han, J. H.; Kim, K. C.; Lee, M. H.; Lutz, L.; Malinin, A. [Institute for Physical Science and Technology, University of Maryland, College Park, MD 20742 (United States); Allison, P.; Beatty, J. J. [Department of Physics, Ohio State University, Columbus, OH 43210 (United States); Bagliesi, M. G.; Bigongiari, G.; Maestro, P.; Marrocchesi, P. S. [Department of Physics, University of Siena and INFN, Siena 53100 (Italy); Childers, J. T.; DuVernois, M. A. [School of Physics and Astronomy, University of Minnesota, MN 55414 (United States); Conklin, N. B.; Coutu, S.; Mognet, S. I. [Department of Physics, Penn State University, University Park, PA 16802 (United States); Jeon, J. A. [Department of Physics, Ewha Womans University, Seoul 120-750 (Korea, Republic of); Minnick, S. [Department of Physics, Kent State University Tuscarawas, New Philadelphia, OH 44663 (United States)], E-mail: seo@umd.edu (and others)

2010-05-01T23:59:59.000Z

330

A COSMIC BATTERY RECONSIDERED G. S. Bisnovatyi-Kogan  

E-Print Network (OSTI)

A COSMIC BATTERY RECONSIDERED G. S. Bisnovatyi-Kogan Space Research Institute, Russian Academy: magnetic fields -- X-rays: stars 1. INTRODUCTION The classical battery mechanism of magnetic field genera currents and an associated magnetic field. Self-induction is very impor- tant in the battery mechanism

331

Signature of cosmic string wakes in the CMB polarization  

Science Conference Proceedings (OSTI)

We calculate a signature of cosmic strings in the polarization of the cosmic microwave background. We find that ionization in the wakes behind moving strings gives rise to extra polarization in a set of rectangular patches in the sky whose length distribution is scale-invariant. The length of an individual patch is set by the comoving Hubble radius at the time the string is perturbing the cosmic microwave background. The polarization signal is largest for string wakes produced at the earliest post-recombination time, and for an alignment in which the photons cross the wake close to the time the wake is created. The maximal amplitude of the polarization relative to the temperature quadrupole is set by the overdensity of free electrons inside a wake which depends on the ionization fraction f inside the wake. For a cosmic string wake coming from an idealized string segment, the signal can be as high as 0.06 {mu}K in degree scale polarization for a string at high redshift (near recombination) and a string tension {mu} given by G{mu}=10{sup -7}.

Danos, Rebecca J.; Brandenberger, Robert H.; Holder, Gil [Department of Physics, McGill University, Montreal, QC, H3A 2T8 (Canada)

2010-07-15T23:59:59.000Z

332

Monte Carlo Simulations of Cosmic Rays Hadronic Interactions  

Science Conference Proceedings (OSTI)

This document describes the construction and results of the MaCoR software tool, developed to model the hadronic interactions of cosmic rays with different geometries of materials. The ubiquity of cosmic radiation in the environment results in the activation of stable isotopes, referred to as cosmogenic activities. The objective is to use this application in conjunction with a model of the MAJORANA DEMONSTRATOR components, from extraction to deployment, to evaluate cosmogenic activation of such components before and after deployment. The cosmic ray showers include several types of particles with a wide range of energy (MeV to GeV). It is infeasible to compute an exact result with a deterministic algorithm for this problem; Monte Carlo simulations are a more suitable approach to model cosmic ray hadronic interactions. In order to validate the results generated by the application, a test comparing experimental muon flux measurements and those predicted by the application is presented. The experimental and simulated results have a deviation of 3%.

Aguayo Navarrete, Estanislao; Orrell, John L.; Kouzes, Richard T.

2011-04-01T23:59:59.000Z

333

Charged Vacuum Condensate Near a Superconducting Cosmic String  

E-Print Network (OSTI)

A charged superconductiong cosmic string produces an extremely large electric field in its vicinity. This leads to vacuum instability and to the formation of a charged vacuum condensate which screens the electric charge of the string. We analyze the structure of this condensate using the Thomas-Fermi method.

J. R. S. Nascimento; Inyong Cho; Alexander Vilenkin

1999-02-18T23:59:59.000Z

334

ORIGIN: metal creation and evolution from the cosmic dawn  

E-Print Network (OSTI)

ORIGIN is a proposal for the M3 mission call of ESA aimed at the study of metal creation from the epoch of cosmic dawn. Using high-spectral resolution in the soft X-ray band, ORIGIN will be able to identify the physical ...

Figueroa-Feliciano, Enectali

335

The cosmic shear STIS parallel program - First results  

E-Print Network (OSTI)

Since the Universe is inhomogeneous on scales well below the Hubble radius, light bundles from distant galaxies are deflected and distorted by the tidal gravitational field of the large-scale matter distribution as they propagate through the Universe. Two-point statistical measures of the observed ellipticities, like the dispersion within a finite aperture or the ellipticity cross-correlation, can be related to the power spectrum of the large-scale structure. The measurement of cosmic shear (especially on small angular scales) can thus be used to constrain cosmological parameters and to test cosmological structure formation in the non-linear regime, without any assumptions about the relation between luminous and dark matter. In this paper we will present preliminary cosmic shear measurements on sub-arcminute scales, obtained from archival STIS parallel data. The high angular resolution of HST, together with the sensitivity and PSF-stability of STIS, allows us to measure cosmic shear along many independent lines-of-sight. Ongoing STIS parallel observations, currently being carried out in the frame of a big GO program (8562+9248), will greatly increase the number of available useful fields and will enable us to measure cosmic shear with higher accuracy on sub-arcminute scales.

H. Haemmerle; J. -M. Miralles; P. Schneider; T. Erben; R. A. E. Fosbury; W. Freudling; N. Pirzkal; S. D. M. White

2001-09-21T23:59:59.000Z

336

Intense low energy positron beams  

Science Conference Proceedings (OSTI)

Intense positron beams are under development or being considered at several laboratories. Already today a few accelerator based high intensity, low brightness e{sup +} beams exist producing of the order of 10{sup 8} {minus} 10{sup 9} e{sup +}/sec. Several laboratories are aiming at high intensity, high brightness e{sup +} beams with intensities greater than 10{sup 9} e{sup +}/sec and current densities of the order of 10{sup 13} {minus} 10{sup 14} e{sup +} sec{sup {minus}} {sup 1}cm{sup {minus}2}. Intense e{sup +} beams can be realized in two ways (or in a combination thereof) either through a development of more efficient B{sup +} moderators or by increasing the available activity of B{sup +} particles. In this review we shall mainly concentrate on the latter approach. In atomic physics the main trust for these developments is to be able to measure differential and high energy cross-sections in e{sup +} collisions with atoms and molecules. Within solid state physics high intensity, high brightness e{sup +} beams are in demand in areas such as the re-emission e{sup +} microscope, two dimensional angular correlation of annihilation radiation, low energy e{sup +} diffraction and other fields. Intense e{sup +} beams are also important for the development of positronium beams, as well as exotic experiments such as Bose condensation and Ps liquid studies.

Lynn, K.G.; Jacobsen, F.M.

1993-12-31T23:59:59.000Z

337

High-Intensity Discharge Lighting  

Energy.gov (U.S. Department of Energy (DOE))

High-intensity discharge (HID) lighting provides the highest efficacy and longest service life of any lighting type. It can save 75%-90% of lighting energy when it replaces incandescent lighting.

338

Neutral particle beam intensity controller  

DOE Patents (OSTI)

The neutral beam intensity controller is based on selected magnetic defocusing of the ion beam prior to neutralization. The defocused portion of the beam is dumped onto a beam dump disposed perpendicular to the beam axis. Selective defocusing is accomplished by means of a magnetic field generator disposed about the neutralizer so that the field is transverse to the beam axis. The magnetic field intensity is varied to provide the selected partial beam defocusing of the ions prior to neutralization. The desired focused neutral beam portion passes along the beam path through a defining aperture in the beam dump, thereby controlling the desired fraction of neutral particles transmitted to a utilization device without altering the kinetic energy level of the desired neutral particle fraction. By proper selection of the magnetic field intensity, virtually zero through 100% intensity control of the neutral beam is achieved.

Dagenhart, W.K.

1984-05-29T23:59:59.000Z

339

Gamma radiation field intensity meter  

DOE Patents (OSTI)

A gamma radiation intensity meter measures dose rate of a radiation field. The gamma radiation intensity meter includes a tritium battery emitting beta rays generating a current which is essentially constant. Dose rate is correlated to an amount of movement of an electroscope element charged by the tritium battery. Ionizing radiation decreases the voltage at the element and causes movement. A bleed resistor is coupled between the electroscope support element or electrode and the ionization chamber wall electrode. 4 figs.

Thacker, L.H.

1994-08-16T23:59:59.000Z

340

Gamma radiation field intensity meter  

DOE Patents (OSTI)

A gamma radiation intensity meter measures dose rate of a radiation field. The gamma radiation intensity meter includes a tritium battery emitting beta rays generating a current which is essentially constant. Dose rate is correlated to an amount of movement of an electroscope element charged by the tritium battery. Ionizing radiation decreases the voltage at the element and causes movement. A bleed resistor is coupled between the electroscope support element or electrode and the ionization chamber wall electrode. 4 figs.

Thacker, L.H.

1995-10-17T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


341

High intensity protons in RHIC  

SciTech Connect

During the 2012 summer shutdown a pair of electron lenses will be installed in RHIC, allowing the beam-beam parameter to be increased by roughly 50 percent. To realize the corresponding luminosity increase bunch intensities have to be increased by 50 percent, to 2.5 {center_dot} 10{sup 11} protons per bunch. We list the various RHIC subsystems that are most affected by this increase, and propose beam studies to ensure their readiness. The proton luminosity in RHIC is presently limited by the beam-beam effect. To overcome this limitation, electron lenses will be installed in IR10. With the help of these devices, the headon beam-beam kick experienced during proton-proton collisions will be partially compensated, allowing for a larger beam-beam tuneshift at these collision points, and therefore increasing the luminosity. This will be accomplished by increasing the proton bunch intensity from the presently achieved 1.65 {center_dot} 10{sup 11} protons per bunch in 109 bunches per beam to 2.5 {center_dot} 10{sup 11}, thus roughly doubling the luminosity. In a further upgrade we aim for bunch intensities up to 3 {center_dot} 10{sup 11} protons per bunch. With RHIC originally being designed for a bunch intensity of 1 {center_dot} 10{sup 11} protons per bunch in 56 bunches, this six-fold increase in the total beam intensity by far exceeds the design parameters of the machine, and therefore potentially of its subsystems. In this note, we present a list of major subsystems that are of potential concern regarding this intensity upgrade, show their demonstrated performance at present intensities, and propose measures and beam experiments to study their readiness for the projected future intensities.

Montag, C.; Ahrens& #44; L.; Blaskiewicz& #44; M.; Brennan& #44; J.M.; Drees& #44; K.A.; Fischer& #44; W.; Huang& #44; H.; Minty& #44; M.; Robert-Demolaize& #44; G.; Thieberger& #44; P.; Yip& #44; K.

2012-01-05T23:59:59.000Z

342

Gamma radiation field intensity meter  

SciTech Connect

A gamma radiation intensity meter measures dose rate of a radiation field. The gamma radiation intensity meter includes a tritium battery emitting beta rays generating a current which is essentially constant. Dose rate is correlated to an amount of movement of an electroscope element charged by the tritium battery. Ionizing radiation decreases the voltage at the element and causes movement. A bleed resistor is coupled between the electroscope support element or electrode and the ionization chamber wall electrode.

Thacker, Louis H. (Knoxville, TN)

1995-01-01T23:59:59.000Z

343

Gamma radiation field intensity meter  

SciTech Connect

A gamma radiation intensity meter measures dose rate of a radiation field. The gamma radiation intensity meter includes a tritium battery emitting beta rays generating a current which is essentially constant. Dose rate is correlated to an amount of movement of an electroscope element charged by the tritium battery. Ionizing radiation decreases the voltage at the element and causes movement. A bleed resistor is coupled between the electroscope support element or electrode and the ionization chamber wall electrode.

Thacker, Louis H. (Knoxville, TN)

1994-01-01T23:59:59.000Z

344

Harmonic generation at high intensities  

Science Conference Proceedings (OSTI)

Atomic electrons subject to intense laser fields can absorb many photons, leading either to multiphoton ionization or the emission of a single, energetic photon which can be a high multiple of the laser frequency. The latter process, high-order harmonic generation, has been observed experimentally using a range of laser wavelengths and intensities over the past several years. Harmonic generation spectra have a generic form: a steep decline for the low order harmonics, followed by a plateau extending to high harmonic order, and finally an abrupt cutoff beyond which no harmonics are discernible. During the plateau the harmonic production is a very weak function of the process order. Harmonic generation is a promising source of coherent, tunable radiation in the XUV to soft X-ray range which could have a variety of scientific and possibly technological applications. Its conversion from an interesting multiphoton phenomenon to a useful laboratory radiation source requires a complete understanding of both its microscopic and macroscopic aspects. We present some recent results on the response of single atoms at intensities relevant to the short pulse experiments. The calculations employ time-dependent methods, which we briefly review in the next section. Following that we discuss the behavior of the harmonics as a function of laser intensity. Two features are notable: the slow scaling of the harmonic intensities with laser intensity, and the rapid variation in the phase of the individual harmonics with respect to harmonic order. We then give a simple empirical formula that predicts the extent of the plateau for a given ionization potential, wavelength and intensity.

Schafer, K.J.; Krause, J.L.; Kulander, K.C.

1993-06-01T23:59:59.000Z

345

Differential Microwave Radiometer and the Cosmic Microwave Background |  

Office of Science (SC) Website

Differential Differential Microwave Radiometer and the Cosmic Microwave Background Laboratory Policy and Evaluation (LPE) LPE Home Staff M&O Contracts SC Laboratory Appraisal Process Laboratory Planning Process Work for Others in the Office of Science Laboratory Directed Research and Development (LDRD) DOE's Philosophy on LDRD Frequently Asked Questions Success Stories Brochures Additional Information LDRD Program Contacts Technology Transfer DOE National Laboratories Contact Information Laboratory Policy and Evaluation U.S. Department of Energy SC-32/Forrestal Building 1000 Independence Ave., SW Washington, DC 20585 P: (202) 586-5447 F: (202) 586-3119 Success Stories Differential Microwave Radiometer and the Cosmic Microwave Background Print Text Size: A A A RSS Feeds FeedbackShare Page

346

The Unified First law in "Cosmic Triad" Vector Field Scenario  

E-Print Network (OSTI)

In this letter, we try to apply the unified first law to the "cosmic triad" vector field scenario both in the minimal coupling case and in the non-minimalcoupling case. After transferring the non-minimally coupling action in Jordan frame to Einstein frame, the correct dynamical equation (Friedmann equation) is gotten in a thermal equilibrium process by using the already existing entropy while the entropy in the non-minimal coupled "cosmic triad" scenario has not been derived. And after transferring the variables back to Jordan frame, the corresponding Friedmann equation is demonstrated to be correct. For complete arguments, we also calculate the related Misner-Sharp energy in Jordan and Einstein frames.

Yi Zhang; Yungui Gong; Zong-Hong Zhu

2011-08-04T23:59:59.000Z

347

Cosmic-Ray Positrons: Are There Primary Sources?  

E-Print Network (OSTI)

Cosmic rays at the Earth include a secondary component originating in collisions of primary particles with the diffuse interstellar gas. The secondary cosmic rays are relatively rare but carry important information on the Galactic propagation of the primary particles. The secondary component includes a small fraction of antimatter particles, positrons and antiprotons. In addition, positrons and antiprotons may also come from unusual sources and possibly provide insight into new physics. For instance, the annihilation of heavy supersymmetric dark matter particles within the Galactic halo could lead to positrons or antiprotons with distinctive energy signatures. With the High-Energy Antimatter Telescope (HEAT) balloon-borne instrument, we have measured the abundances of positrons and electrons at energies between 1 and 50 GeV. The data suggest that indeed a small additional antimatter component may be present that cannot be explained by a purely secondary production mechanism. Here we describe the signature of the effect and discuss its possible origin.

Stephane Coutu; Steven W. Barwick; James J. Beatty; Amit Bhattacharyya; Chuck R. Bower; Christopher J. Chaput; Georgia A. de Nolfo; Michael A. DuVernois; Allan Labrador; Shawn P. McKee; Dietrich Muller; James A. Musser; Scott L. Nutter; Eric Schneider; Simon P. Swordy; Gregory Tarle; Andrew D. Tomasch; Eric Torbet

1999-02-10T23:59:59.000Z

348

ON THE ORIGIN OF THE SOLAR COMPONENT OF COSMIC RADIATION  

SciTech Connect

Ascending prominences in the outer corona often reach velocities above 600 km/sec, 3 times the thermal velocity of coronal protons. lt is not probable that such prominences move through the corona. lt seems much more probable that prominences and the surrounding corona are lifted together by the sarne force. Coronal films give some evidence in this direction. There can be no doubt thai the acceleration force is of a magnetic nature. Under such circumstances, a kind of hollow cavity is formed. Such low-density cavities represent very favorable conditions for the acceleration of cosmic particles. This type of mechanism has the advantage of explaining in a natural way the observed delay between the begirning of a flare and the terrestrial onset of the cosmic-ray burst. (A.C.)

Kiepenheuer, K.O.

1958-01-01T23:59:59.000Z

349

A Fast Algorithm for Cosmic Rays Removal from Single Images  

E-Print Network (OSTI)

We present a method for detecting cosmic rays in single images. The algorithm is based on simple analysis of the histogram of the image data and does not use any modeling of the picture of the object. It does not require a good signal to noise ratio in the image data. Identification of multiple-pixel cosmic-ray hits is realized by running the procedure for detection and replacement iteratively. The tests performed by us, show that the method is very effective, when applied to the images with the spectroscopic data. It is also very fast in comparison with other single image algorithms found in astronomical data processing packages. Practical implementation and examples of application are presented.

Wojtek Pych

2003-11-12T23:59:59.000Z

350

Search for Correlated High Energy Cosmic Ray Events with CHICOS  

E-Print Network (OSTI)

We present the results of a search for time correlations in high energy cosmic ray data (primary E > 10^{14} eV) collected by the California HIgh school Cosmic ray ObServatory (CHICOS) array. Data from 60 detector sites spread over an area of 400 km^2 were studied for evidence of correlated events separated by more than 1 km with coincidence times ranging from 1 microsec up to 1 second. All searches were consistent with the absence of excess coincidences except for a 2.9 sigma excess observed for coincidence times less than 10 microsec. We report upper limits for the coincidence probability as a function of coincidence time.

Carlson, B E; Jillings, C J; Larson, M B; Lynn, T W; McKeown, R D; Hill, J E; Falkowski, B J; Seki, R; Sepikas, J; Yodh, G B; Hill, James E.

2005-01-01T23:59:59.000Z

351

CMB Anisotropy Induced by a Moving Straight Cosmic String  

E-Print Network (OSTI)

We showed that the part of strings could be detected by optical method is only 20% from the total available amount of such objects, therefore the gravitational lensing method has to be "completed" by CMB one. We found the general structure of the CMB anisotropy generated by a cosmic string for simple model of straight string moving with constant velocity. For strings with deficit angle 1-2 arcsec the amplitude of generated anisotropy has to be 15-30 muK (the corresponding string linear density is (G mu) ~ 10^{-7} and energy is GUT one, 10^{15} GeV). To use both radio and optical methods the deficit angle has to be from 0.1 arcsec to 5-6 arcsec. If cosmic string can be detected by optical method, the length of corresponding brightness spot of anisotropy has to be no less than 100 degrees.

O. S. Sazhina; M. V. Sazhin; V. N. Sementsov; M. Capaccioli; G. Longo; G. Riccio; G. D'Angelo

2008-09-05T23:59:59.000Z

352

Low Energy Cosmic Rays and the Disturbed Magnetosphere  

E-Print Network (OSTI)

Low energy galactic cosmic rays as well as particles accelerated to high energies either at the solar surface or in the interplanetary medium have access to the atmosphere above a given position on the Earth depending upon the state of the magnetosphere. The interpretation of the cosmic ray anisotropy, deduced from the neutron monitor (NM) network, must assume the variability of the magnetospheric configuration. Along with a short review of changes of the geomagnetic cutoffs in the disturbed magnetosphere reported in the earlier papers, we present the results of computations of transmissivity function and asymptotic directions for selected points on the ground and for a low altitude polar orbiting satellite as well. The computations, based on different available models of geomagnetic field of external sources are performed for quiet time periods and for strong geomagnetic disturbances occurred in 2003 and 2004.

Kudela, K

2013-01-01T23:59:59.000Z

353

Scalar tensor theory : validity of Cosmic no hair conjecture  

E-Print Network (OSTI)

The paper deals with cosmic no hair conjecture in scalar tensor theory of gravity. Here we have considered both Jordan frame and Einstein frame to examine the conjecture. In Jordan frame, one should restrict both the coupling function of the scalar field and the coupling parameter in addition to the ususal energy conditions for the the matter field for the validity of CNHC while in Einstein frame the restrictions are purely on the energy conditions.

Sudeshna Mukerji; Nairwita Mazumder; Ritabrata Biswas; Subenoy Chakraborty

2011-06-09T23:59:59.000Z

354

Gravity assisted dark energy dominance and cosmic acceleration  

E-Print Network (OSTI)

It is proposed that dark energy may become dominant over standard matter due to universe expansion (curvature decrease). Two models: non-linear gravity-matter system and modified gravity may provide the effective phantom or effective quintessence dark energy which complies with the conjecture. It is interesting that future of such universe is not necessary finite time singularity (Big Rip). The effective quintessence naturally describes current cosmic speed-up.

Nojiri, S; Nojiri, Shin'ichi; Odintsov, Sergei D.

2004-01-01T23:59:59.000Z

355

Fine structure constant in the spacetime of a cosmic string  

E-Print Network (OSTI)

We calculate the fine structure constant in the spacetime of a cosmic string. In the presence of a cosmic string the value of the fine structure constant reduces. We also discuss on numerical results. The gravitational properties of cosmic strings are strikingly different from those of non-relativistic linear distributions of matter. To explain the origin of the difference, we note that for a static matter distribution with energymomentum tensor, T µ ? = diag (?, ?p1, ?p2, ?p3) , (1) the Newtonian limit of the Einstein equations become ? 2 ? = 4?G (? + p1 + p2 + p3), (2) where ? is the gravitational potential. For non-relativistic matter, pi ? ? and ? 2 ? = 4?G?. Strings, on the other hand, have a large longitudinal tension. For a straight string parallel to the z-axis, p3 = ??, with p1 and p2 vanish when averaged over the string cross-section. Hence, the righthand side of Eq.(2) vanishes, suggesting that straight strings produce no gravitational forece on surrounding matter. This conclusion is confirmed by a full general-relativistic analysis. Another feature distinguishing cosmic strings from more familiar sources is their relativistic motion. As a result, oscillating loops of string can be strong emitters of gravitational radiation. A gravitating string is described by the combined system of Einstein, Higgs and guage field equations. The problem of solving these coupled equations is formidable and no exact solutions have been found to date. Fortunately, for most cosmological applications the problem can be made tractable by adopting two major simplifications. First, assuming that the string thickness is much smaller than all other relevant dimensions, the string can be 1

Forough Nasseri

2005-01-01T23:59:59.000Z

356

Simulation of Cosmic Ray neutrinos Interactions in Water  

E-Print Network (OSTI)

The program CORSIKA, usually used to simulate extensive cosmic ray air showers, has been adapted to a water medium in order to study the acoustic detection of ultra high energy neutrinos. Showers in water from incident protons and from neutrinos have been generated and their properties are described. The results obtained from CORSIKA are compared to those from other available simulation programs such as Geant4.

T. Sloan

2006-09-21T23:59:59.000Z

357

Interacting Dark Energy and the Cosmic Coincidence Problem  

E-Print Network (OSTI)

The introduction of an interaction for dark energy to the standard cosmology offers a potential solution to the cosmic coincidence problem. We examine the conditions on the dark energy density that must be satisfied for this scenario to be realized. Under some general conditions we find a stable attractor for the evolution of the Universe in the future. Holographic conjectures for the dark energy offer some specific examples of models with the desired properties.

Micheal S. Berger; Hamed Shojaei

2006-01-20T23:59:59.000Z

358

Milagro Contributions to XXVI International Cosmic Ray Conference  

SciTech Connect

Milagrito, a prototype for the Milagro detector, operated for 15 months in 1997--8 and collected 8.9 x 10{sup 9} events. It was the first extensive air shower (EAS) array sensitive to showers initiated by primaries with energy below 1 TeV. The shadows of the sun and moon observed with cosmic rays can be used to study systematic pointing shifts and measure the angular resolution of EAS arrays. Below a few TeV, the paths of cosmic rays coming toward the earth are bent by the helio- and geo-magnetic fields. This is expected to distort and displace the shadows of the sun and the moon. The moon shadow, offset from the nominal (unreflected) position, has been observed with high statistical significance in Milagrito. This can be used to establish energy calibrations, as well as to search for the anti-matter content of the VHE cosmic ray flux. The shadow of the sun has also been observed with high significance.

Hoffman, C.M.; Haines, T.J.; Sinnis, G.; Miller, R.S.; Thompson, N.T.

1999-08-01T23:59:59.000Z

359

Can $f(T)$ gravity theories mimic $?$CDM cosmic history  

E-Print Network (OSTI)

Recently the teleparallel Lagrangian density described by the torsion scalar T has been extended to a function of T. The $f(T)$ modified teleparallel gravity has been proposed as the natural gravitational alternative for dark energy to explain the late time acceleration of the universe. In order to reconstruct the function $f(T)$ by demanding a background $\\Lambda$CDM cosmology we assume that, (i) the background cosmic history provided by the flat $\\Lambda$CDM (the radiation ere with $\\omega_{eff}=1/3$, matter and de Sitter eras with $\\omega_{eff}=0$ and $\\omega_{eff}=-1$, respectively) (ii) the radiation dominate in the radiation era with $\\Omega_{0r}=1$ and the matter dominate during the matter phases when $\\Omega_{0m}=1$. We find the cosmological dynamical system which can obey the $\\Lambda$CDM cosmic history. In each era, we find a critical lines that, the radiation dominated and the matter dominated are one points of them in the radiation and matter phases, respectively. Also, we drive the cosmologically viability condition for these models. We investigate the stability condition with respect to the homogeneous scalar perturbations in each era and we obtain the stability conditions for the fixed points in each eras. Finally, we reconstruct the function $f(T)$ which mimics cosmic expansion history.

M. R. Setare; N. Mohammadipour

2013-01-12T23:59:59.000Z

360

Cosmic-ray Driven Outflows in Global Galaxy Disk Models  

E-Print Network (OSTI)

Galactic-scale winds are a generic feature of massive galaxies with high star formation rates across a broad range of redshifts. Despite their importance, a detailed physical understanding of what drives these mass-loaded global flows has remained elusive. In this paper, we explore the dynamical impact of cosmic rays by performing the first three-dimensional, adaptive mesh refinement simulations of an isolated starbursting galaxy that includes a basic model for the production, dynamics and diffusion of galactic cosmic rays. We find that including cosmic rays naturally leads to robust, massive, bipolar outflows from our 10^12 Msun halo, with a mass-loading factor Mout/SFR = 0.3 for our fiducial run. Other reasonable parameter choices led to mass-loading factors above unity. The wind is multiphase and is accelerated to velocities well in excess of the escape velocity. We employ a two-fluid model for the thermal gas and relativistic CR plasma and model a range of physics relevant to galaxy formation, including r...

Salem, Munier

2013-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


361

Hurricane Maximum Intensity: Past and Present  

Science Conference Proceedings (OSTI)

Hurricane intensity forecasting has lagged far behind the forecasting of hurricane track. In an effort to improve the understanding of the hurricane intensity dilemma, several attempts have been made to compute an upper bound on the intensity of ...

J. Parks Camp; Michael T. Montgomery

2001-07-01T23:59:59.000Z

362

Cosmic Rays from Supernovae Proven to Hit Earth | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Cosmic Rays from Supernovae Proven to Hit Earth Cosmic Rays from Supernovae Proven to Hit Earth Cosmic Rays from Supernovae Proven to Hit Earth March 5, 2013 - 4:40pm Addthis When stars explode, the supernovas send off shock waves like the one shown in this artist's rendition, which accelerate protons to cosmic-ray energies through a process known as Fermi acceleration. Andy Freeberg SLAC National Accelerator Laboratory Did you know? Protons make up 90 percent of the cosmic rays that hit Earth's atmosphere, triggering showers of particles that reach the ground and creating radiation for air travelers. The energies of these protons as they leave the supernovae are far beyond what the most powerful particle colliders on Earth can produce. Cosmic rays, energetic particles that pelt Earth, are born in the violent

363

Constraints on cosmic (super)strings from the LIGO-Virgo gravitational-wave detectors  

E-Print Network (OSTI)

Cosmic string cusps produce powerful bursts of gravitational waves (GWs). These bursts provide the most promising observational signature of cosmic strings. In this letter we report stringent limits on cosmic string models obtained from the analysis of 625 days of observation with the LIGO and Virgo GW detectors. A significant fraction of the cosmic string parameter space is ruled out. This result complements and improves existing limits from searches for a stochastic background of GWs using cosmic microwave background and pulsar timing data. In particular, if the size of loops is given by gravitational back-reaction, we place upper limits on the string tension $G\\mu$ below $10^{-8}$ in some regions of the cosmic string parameter space.

J. Aasi; J. Abadie; B. P. Abbott; R. Abbott; T. Abbott; M. R. Abernathy; T. Accadia; F. Acernese; C. Adams; T. Adams; R. X. Adhikari; C. Affeldt; M. Agathos; N. Aggarwal; O. D. Aguiar; P. Ajith; B. Allen; A. Allocca; E. Amador Ceron; D. Amariutei; R. A. Anderson; S. B. Anderson; W. G. Anderson; K. Arai; M. C. Araya; C. Arceneaux; J. Areeda; S. Ast; S. M. Aston; P. Astone; P. Aufmuth; C. Aulbert; L. Austin; B. E. Aylott; S. Babak; P. T. Baker; G. Ballardin; S. W. Ballmer; J. C. Barayoga; D. Barker; S. H. Barnum; F. Barone; B. Barr; L. Barsotti; M. Barsuglia; M. A. Barton; I. Bartos; R. Bassiri; A. Basti; J. Batch; J. Bauchrowitz; Th. S. Bauer; M. Bebronne; B. Behnke; M. Bejger; M. G. Beker; A. S. Bell; C. Bell; I. Belopolski; G. Bergmann; J. M. Berliner; D. Bersanetti; A. Bertolini; D. Bessis; J. Betzwieser; P. T. Beyersdorf; T. Bhadbhade; I. A. Bilenko; G. Billingsley; J. Birch; M. Bitossi; M. A. Bizouard; E. Black; J. K. Blackburn; L. Blackburn; D. Blair; M. Blom; O. Bock; T. P. Bodiya; M. Boer; C. Bogan; C. Bond; F. Bondu; L. Bonelli; R. Bonnand; R. Bork; M. Born; V. Boschi; S. Bose; L. Bosi; J. Bowers; C. Bradaschia; P. R. Brady; V. B. Braginsky; M. Branchesi; C. A. Brannen; J. E. Brau; J. Breyer; T. Briant; D. O. Bridges; A. Brillet; M. Brinkmann; V. Brisson; M. Britzger; A. F. Brooks; D. A. Brown; D. D. Brown; F. Brückner; T. Bulik; H. J. Bulten; A. Buonanno; D. Buskulic; C. Buy; R. L. Byer; L. Cadonati; G. Cagnoli; J. Calderón Bustillo; E. Calloni; J. B. Camp; P. Campsie; K. C. Cannon; B. Canuel; J. Cao; C. D. Capano; F. Carbognani; L. Carbone; S. Caride; A. Castiglia; S. Caudill; M. Cavagliá; F. Cavalier; R. Cavalieri; G. Cella; C. Cepeda; E. Cesarini; R. Chakraborty; T. Chalermsongsak; S. Chao; P. Charlton; E. Chassande-Mottin; X. Chen; Y. Chen; A. Chincarini; A. Chiummo; H. S. Cho; J. Chow; N. Christensen; Q. Chu; S. S. Y. Chua; S. Chung; G. Ciani; F. Clara; D. E. Clark; J. A. Clark; F. Cleva; E. Coccia; P. -F. Cohadon; A. Colla; M. Colombini; M. Constancio Jr.; A. Conte; R. Conte; D. Cook; T. R. Corbitt; M. Cordier; N. Cornish; A. Corsi; C. A. Costa; M. W. Coughlin; J. -P. Coulon; S. Countryman; P. Couvares; D. M. Coward; M. Cowart; D. C. Coyne; K. Craig; J. D. E. Creighton; T. D. Creighton; S. G. Crowder; A. Cumming; L. Cunningham; E. Cuoco; K. Dahl; T. Dal Canton; M. Damjanic; S. L. Danilishin; S. D'Antonio; K. Danzmann; V. Dattilo; B. Daudert; H. Daveloza; M. Davier; G. S. Davies; E. J. Daw; R. Day; T. Dayanga; R. De Rosa; G. Debreczeni; J. Degallaix; W. Del Pozzo; E. Deleeuw; S. Deléglise; T. Denker; T. Dent; H. Dereli; V. Dergachev; R. DeRosa; R. DeSalvo; S. Dhurandhar; L. Di Fiore; A. Di Lieto; I. Di Palma; A. Di Virgilio; M. Díaz; A. Dietz; K. Dmitry; F. Donovan; K. L. Dooley; S. Doravari; M. Drago; R. W. P. Drever; J. C. Driggers; Z. Du; J. -C. Dumas; S. Dwyer; T. Eberle; M. Edwards; A. Effler; P. Ehrens; J. Eichholz; S. S. Eikenberry; G. Endröczi; R. Essick; T. Etzel; K. Evans; M. Evans; T. Evans; M. Factourovich; V. Fafone; S. Fairhurst; Q. Fang; S. Farinon; B. Farr; W. Farr; M. Favata; D. Fazi; H. Fehrmann; D. Feldbaum; I. Ferrante; F. Ferrini; F. Fidecaro; L. S. Finn; I. Fiori; R. Fisher; R. Flaminio; E. Foley; S. Foley; E. Forsi; N. Fotopoulos; J. -D. Fournier; S. Franco; S. Frasca; F. Frasconi; M. Frede; M. Frei; Z. Frei; A. Freise; R. Frey; T. T. Fricke; P. Fritschel; V. V. Frolov; M. -K. Fujimoto; P. Fulda; M. Fyffe; J. Gair; L. Gammaitoni; J. Garcia; F. Garufi; N. Gehrels; G. Gemme; E. Genin; A. Gennai; L. Gergely; S. Ghosh; J. A. Giaime; S. Giampanis; K. D. Giardina; A. Giazotto; S. Gil-Casanova; C. Gill; J. Gleason; E. Goetz; R. Goetz; L. Gondan; G. González; N. Gordon; M. L. Gorodetsky; S. Gossan; S. Goßler; R. Gouaty; C. Graef; P. B. Graff; M. Granata; A. Grant; S. Gras; C. Gray; R. J. S. Greenhalgh; A. M. Gretarsson; C. Griffo; P. Groot; H. Grote; K. Grover; S. Grunewald; G. M. Guidi; C. Guido; K. E. Gushwa; E. K. Gustafson; R. Gustafson; B. Hall; E. Hall; D. Hammer; G. Hammond; M. Hanke; J. Hanks; C. Hanna; J. Hanson; J. Harms; G. M. Harry; I. W. Harry; E. D. Harstad; M. T. Hartman; K. Haughian; K. Hayama; J. Heefner; A. Heidmann; M. Heintze; H. Heitmann; P. Hello; G. Hemming; M. Hendry; I. S. Heng; A. W. Heptonstall; M. Heurs; S. Hild; D. Hoak; K. A. Hodge; K. Holt; M. Holtrop; T. Hong; S. Hooper; T. Horrom; D. J. Hosken; J. Hough; E. J. Howell; Y. Hu; Z. Hua; V. Huang; E. A. Huerta; B. Hughey; S. Husa; S. H. Huttner; M. Huynh; T. Huynh-Dinh; J. Iafrate; D. R. Ingram; R. Inta; T. Isogai; A. Ivanov; B. R. Iyer; K. Izumi; M. Jacobson; E. James; H. Jang; Y. J. Jang; P. Jaranowski; F. Jiménez-Forteza; W. W. Johnson; D. Jones; D. I. Jones; R. Jones; R. J. G. Jonker; L. Ju; Haris K; P. Kalmus; V. Kalogera; S. Kandhasamy; G. Kang; J. B. Kanner; M. Kasprzack; R. Kasturi; E. Katsavounidis; W. Katzman; H. Kaufer; K. Kaufman; K. Kawabe; S. Kawamura; F. Kawazoe

2013-10-09T23:59:59.000Z

364

Constraints on cosmic (super)strings from the LIGO-Virgo gravitational-wave detectors  

E-Print Network (OSTI)

Cosmic string cusps produce powerful bursts of gravitational waves (GWs). These bursts provide the most promising observational signature of cosmic strings. In this letter we report stringent limits on cosmic string models obtained from the analysis of 625 days of observation with the LIGO and Virgo GW detectors. A significant fraction of the cosmic string parameter space is ruled out. This result complements and improves existing limits from searches for a stochastic background of GWs using cosmic microwave background and pulsar timing data. In particular, if the size of loops is given by gravitational back-reaction, we place upper limits on the string tension $G\\mu$ below $10^{-8}$ in some regions of the cosmic string parameter space.

Aasi, J; Abbott, B P; Abbott, R; Abbott, T; Abernathy, M R; Accadia, T; Acernese, F; Adams, C; Adams, T; Adhikari, R X; Affeldt, C; Agathos, M; Aggarwal, N; Aguiar, O D; Ajith, P; Allen, B; Allocca, A; Ceron, E Amador; Amariutei, D; Anderson, R A; Anderson, S B; Anderson, W G; Arai, K; Araya, M C; Arceneaux, C; Areeda, J; Ast, S; Aston, S M; Astone, P; Aufmuth, P; Aulbert, C; Austin, L; Aylott, B E; Babak, S; Baker, P T; Ballardin, G; Ballmer, S W; Barayoga, J C; Barker, D; Barnum, S H; Barone, F; Barr, B; Barsotti, L; Barsuglia, M; Barton, M A; Bartos, I; Bassiri, R; Basti, A; Batch, J; Bauchrowitz, J; Bauer, Th S; Bebronne, M; Behnke, B; Bejger, M; Beker, M G; Bell, A S; Bell, C; Belopolski, I; Bergmann, G; Berliner, J M; Bersanetti, D; Bertolini, A; Bessis, D; Betzwieser, J; Beyersdorf, P T; Bhadbhade, T; Bilenko, I A; Billingsley, G; Birch, J; Bitossi, M; Bizouard, M A; Black, E; Blackburn, J K; Blackburn, L; Blair, D; Blom, M; Bock, O; Bodiya, T P; Boer, M; Bogan, C; Bond, C; Bondu, F; Bonelli, L; Bonnand, R; Bork, R; Born, M; Boschi, V; Bose, S; Bosi, L; Bowers, J; Bradaschia, C; Brady, P R; Braginsky, V B; Branchesi, M; Brannen, C A; Brau, J E; Breyer, J; Briant, T; Bridges, D O; Brillet, A; Brinkmann, M; Brisson, V; Britzger, M; Brooks, A F; Brown, D A; Brown, D D; Brückner, F; Bulik, T; Bulten, H J; Buonanno, A; Buskulic, D; Buy, C; Byer, R L; Cadonati, L; Cagnoli, G; Bustillo, J Calderón; Calloni, E; Camp, J B; Campsie, P; Cannon, K C; Canuel, B; Cao, J; Capano, C D; Carbognani, F; Carbone, L; Caride, S; Castiglia, A; Caudill, S; Cavagliá, M; Cavalier, F; Cavalieri, R; Cella, G; Cepeda, C; Cesarini, E; Chakraborty, R; Chalermsongsak, T; Chao, S; Charlton, P; Chassande-Mottin, E; Chen, X; Chen, Y; Chincarini, A; Chiummo, A; Cho, H S; Chow, J; Christensen, N; Chu, Q; Chua, S S Y; Chung, S; Ciani, G; Clara, F; Clark, D E; Clark, J A; Cleva, F; Coccia, E; Cohadon, P -F; Colla, A; Colombini, M; Constancio, M; Conte, A; Conte, R; Cook, D; Corbitt, T R; Cordier, M; Cornish, N; Corsi, A; Costa, C A; Coughlin, M W; Coulon, J -P; Countryman, S; Couvares, P; Coward, D M; Cowart, M; Coyne, D C; Craig, K; Creighton, J D E; Creighton, T D; Crowder, S G; Cumming, A; Cunningham, L; Cuoco, E; Dahl, K; Canton, T Dal; Damjanic, M; Danilishin, S L; D'Antonio, S; Danzmann, K; Dattilo, V; Daudert, B; Daveloza, H; Davier, M; Davies, G S; Daw, E J; Day, R; Dayanga, T; De Rosa, R; Debreczeni, G; Degallaix, J; Del Pozzo, W; Deleeuw, E; Deléglise, S; Denker, T; Dent, T; Dereli, H; Dergachev, V; DeRosa, R; DeSalvo, R; Dhurandhar, S; Di Fiore, L; Di Lieto, A; Di Palma, I; Di Virgilio, A; Díaz, M; Dietz, A; Dmitry, K; Donovan, F; Dooley, K L; Doravari, S; Drago, M; Drever, R W P; Driggers, J C; Du, Z; Dumas, J -C; Dwyer, S; Eberle, T; Edwards, M; Effler, A; Ehrens, P; Eichholz, J; Eikenberry, S S; Endröczi, G; Essick, R; Etzel, T; Evans, K; Evans, M; Evans, T; Factourovich, M; Fafone, V; Fairhurst, S; Fang, Q; Farinon, S; Farr, B; Farr, W; Favata, M; Fazi, D; Fehrmann, H; Feldbaum, D; Ferrante, I; Ferrini, F; Fidecaro, F; Finn, L S; Fiori, I; Fisher, R; Flaminio, R; Foley, E; Foley, S; Forsi, E; Fotopoulos, N; Fournier, J -D; Franco, S; Frasca, S; Frasconi, F; Frede, M; Frei, M; Frei, Z; Freise, A; Frey, R; Fricke, T T; Fritschel, P; Frolov, V V; Fujimoto, M -K; Fulda, P; Fyffe, M; Gair, J; Gammaitoni, L; Garcia, J; Garufi, F; Gehrels, N; Gemme, G; Genin, E; Gennai, A; Gergely, L; Ghosh, S; Giaime, J A; Giampanis, S; Giardina, K D; Giazotto, A; Gil-Casanova, S; Gill, C; Gleason, J; Goetz, E; Goetz, R; Gondan, L; González, G; Gordon, N; Gorodetsky, M L; Gossan, S; Goßler, S; Gouaty, R; Graef, C; Graff, P B; Granata, M; Grant, A; Gras, S; Gray, C; Greenhalgh, R J S; Gretarsson, A M; Griffo, C; Groot, P; Grote, H; Grover, K; Grunewald, S; Guidi, G M; Guido, C; Gushwa, K E; Gustafson, E K; Gustafson, R; Hall, B; Hall, E; Hammer, D; Hammond, G; Hanke, M; Hanks, J; Hanna, C; Hanson, J; Harms, J; Harry, G M; Harry, I W; Harstad, E D; Hartman, M T; Haughian, K; Hayama, K; Heefner, J; Heidmann, A; Heintze, M; Heitmann, H; Hello, P; Hemming, G; Hendry, M; Heng, I S; Heptonstall, A W; Heurs, M; Hild, S; Hoak, D; Hodge, K A; Holt, K; Holtrop, M; Hong, T; Hooper, S; Horrom, T; Hosken, D J; Hough, J; Howell, E J; Hu, Y; Hua, Z; Huang, V; Huerta, E A; Hughey, B; Husa, S; Huttner, S H; Huynh, M; Huynh-Dinh, T; Iafrate, J; Ingram, D R; Inta, R; Isogai, T; Ivanov, A; Iyer, B R; Izumi, K; Jacobson, M; James, E; Jang, H; Jang, Y J; Jaranowski, P; Jiménez-Forteza, F; Johnson, W W; Jones, D; Jones, D I; Jones, R; Jonker, R J G; Ju, L; K, Haris; Kalmus, P; Kalogera, V; Kandhasamy, S; Kang, G; Kanner, J B; Kasprzack, M; Kasturi, R; Katsavounidis, E; Katzman, W; Kaufer, H; Kaufman, K; Kawabe, K; Kawamura, S; Kawazoe, F; Kéfélian, F; Keitel, D; Kelley, D B; Kells, W; Keppel, D G; Khalaidovski, A; Khalili, F Y; Khazanov, E A; Kim, B K; Kim, C; Kim, K

2013-01-01T23:59:59.000Z

365

Neutral particle beam intensity controller  

DOE Patents (OSTI)

A neutral beam intensity controller is provided for a neutral beam generator in which a neutral beam is established by accelerating ions from an ion source into a gas neutralizer. An amplitude modulated, rotating magnetic field is applied to the accelerated ion beam in the gas neutralizer to defocus the resultant neutral beam in a controlled manner to achieve intensity control of the neutral beam along the beam axis at constant beam energy. The rotating magnetic field alters the orbits of ions in the gas neutralizer before they are neutralized, thereby controlling the fraction of neutral particles transmitted out of the neutralizer along the central beam axis to a fusion device or the like. The altered path or defocused neutral particles are sprayed onto an actively cooled beam dump disposed perpendicular to the neutral beam axis and having a central open for passage of the focused beam at the central axis of the beamline. Virtually zero therough 100% intensity control is achieved by varying the magnetic field strength without altering the ion source beam intensity or its species yield.

Dagenhart, William K. (Oak Ridge, TN)

1986-01-01T23:59:59.000Z

366

Changes in Energy Intensity 1985-1991  

Annual Energy Outlook 2012 (EIA)

Information Administration Home Page. Home > Energy Users > Manufacturing > Changes in Energy Intensity Changes in Energy Intensity 1985-1991 Overview Full Report The focus is...

367

Catalysis Center for Energy Innovation (CCEI): YouTube Channel for this Energy Frontier Research Center (EFRC)  

DOE Data Explorer (OSTI)

CCEI is among the 46 Energy Frontier Research Centers (EFRCs) funded by DOE and was established in the spring of 2009. CCEI is one of the very few externally funded centers on heterogeneous catalysis. CCEI leverages federal funding to enable technology transfer and commercialization through an industrial consortium. The center builds upon the long tradition of the Center for Catalytic Science and Technology (CCST) at the University of Delaware and extends its expertise within a virtual center among multiple partner institutions and national labs (University of Pennsylvania, Caltech, University of Minnesota, University of Massachusetts, Lehigh University, Brookhaven National Labs, University of North Carolina, and University of Southern California). CCEI provides an integrated approach to solving scientific and engineering problems that span across scales and disciplines, ranging from synthesis and characterization of novel catalysts to development and application of a multiscale modeling toolbox to reaction and reactor evaluation to technology transfer.[Copied with editing from http://www.youtube.com/catalysiscenter#p/u

368

The Pierre Auger Observatory II: Studies of Cosmic Ray Composition and Hadronic Interaction models  

E-Print Network (OSTI)

Studies of the composition of the highest energy cosmic rays with the Pierre Auger Observatory, including examination of hadronic physics effects on the structure of extensive air showers.

The Pierre Auger Collaboration; P. Abreu; M. Aglietta; E. J. Ahn; I. F. M. Albuquerque; D. Allard; I. Allekotte; J. Allen; P. Allison; J. Alvarez Castillo; J. Alvarez-Muñiz; M. Ambrosio; A. Aminaei; L. Anchordoqui; S. Andringa; T. Anti?i?; A. Anzalone; C. Aramo; E. Arganda; F. Arqueros; H. Asorey; P. Assis; J. Aublin; M. Ave; M. Avenier; G. Avila; T. Bäcker; M. Balzer; K. B. Barber; A. F. Barbosa; R. Bardenet; S. L. C. Barroso; B. Baughman; J. Bäuml; J. J. Beatty; B. R. Becker; K. H. Becker; A. Bellétoile; J. A. Bellido; S. BenZvi; C. Berat; X. Bertou; P. L. Biermann; P. Billoir; F. Blanco; M. Blanco; C. Bleve; H. Blümer; M. Bohá?ová; D. Boncioli; C. Bonifazi; R. Bonino; N. Borodai; J. Brack; P. Brogueira; W. C. Brown; R. Bruijn; P. Buchholz; A. Bueno; R. E. Burton; K. S. Caballero-Mora; L. Caramete; R. Caruso; A. Castellina; O. Catalano; G. Cataldi; L. Cazon; R. Cester; J. Chauvin; S. H. Cheng; A. Chiavassa; J. A. Chinellato; A. Chou; J. Chudoba; R. W. Clay; M. R. Coluccia; R. Conceição; F. Contreras; H. Cook; M. J. Cooper; J. Coppens; A. Cordier; U. Cotti; S. Coutu; C. E. Covault; A. Creusot; A. Criss; J. Cronin; A. Curutiu; S. Dagoret-Campagne; R. Dallier; S. Dasso; K. Daumiller; B. R. Dawson; R. M. de Almeida; M. De Domenico; C. De Donato; S. J. de Jong; G. De La Vega; W. J. M. de Mello Junior; J. R. T. de Mello Neto; I. De Mitri; V. de Souza; K. D. de Vries; G. Decerprit; L. del Peral; O. Deligny; H. Dembinski; N. Dhital; C. Di Giulio; J. C. Diaz; M. L. Díaz Castro; P. N. Diep; C. Dobrigkeit; W. Docters; J. C. D'Olivo; P. N. Dong; A. Dorofeev; J. C. dos Anjos; M. T. Dova; D. D'Urso; I. Dutan; J. Ebr; R. Engel; M. Erdmann; C. O. Escobar; A. Etchegoyen; P. Facal San Luis; I. Fajardo Tapia; H. Falcke; G. Farrar; A. C. Fauth; N. Fazzini; A. P. Ferguson; A. Ferrero; B. Fick; A. Filevich; A. Filip?i?; S. Fliescher; C. E. Fracchiolla; E. D. Fraenkel; U. Fröhlich; B. Fuchs; R. Gaior; R. F. Gamarra; S. Gambetta; B. García; D. García Gámez; D. Garcia-Pinto; A. Gascon; H. Gemmeke; K. Gesterling; P. L. Ghia; U. Giaccari; M. Giller; H. Glass; M. S. Gold; G. Golup; F. Gomez Albarracin; M. Gómez Berisso; P. Gonçalves; D. Gonzalez; J. G. Gonzalez; B. Gookin; D. Góra; A. Gorgi; P. Gouffon; S. R. Gozzini; E. Grashorn; S. Grebe; N. Griffith; M. Grigat; A. F. Grillo; Y. Guardincerri; F. Guarino; G. P. Guedes; A. Guzman; J. D. Hague; P. Hansen; D. Harari; S. Harmsma; J. L. Harton; A. Haungs; T. Hebbeker; D. Heck; A. E. Herve; C. Hojvat; N. Hollon; V. C. Holmes; P. Homola; J. R. Hörandel; A. Horneffer; M. Hrabovský; T. Huege; A. Insolia; F. Ionita; A. Italiano; C. Jarne; S. Jiraskova; M. Josebachuili; K. Kadija; K. -H. Kampert; P. Karhan; P. Kasper; B. Kégl; B. Keilhauer; A. Keivani; J. L. Kelley; E. Kemp; R. M. Kieckhafer; H. O. Klages; M. Kleifges; J. Kleinfeller; J. Knapp; D. -H. Koang; K. Kotera; N. Krohm; O. Krömer; D. Kruppke-Hansen; F. Kuehn; D. Kuempel; J. K. Kulbartz; N. Kunka; G. La Rosa; C. Lachaud; P. Lautridou; M. S. A. B. Leão; D. Lebrun; P. Lebrun; M. A. Leigui de Oliveira; A. Lemiere; A. Letessier-Selvon; I. Lhenry-Yvon; K. Link; R. López; A. Lopez Agüera; K. Louedec; J. Lozano Bahilo; A. Lucero; M. Ludwig; H. Lyberis; M. C. Maccarone; C. Macolino; S. Maldera; D. Mandat; P. Mantsch; A. G. Mariazzi; J. Marin; V. Marin; I. C. Maris; H. R. Marquez Falcon; G. Marsella; D. Martello; L. Martin; H. Martinez; O. Martínez Bravo; H. J. Mathes; J. Matthews; J. A. J. Matthews; G. Matthiae; D. Maurizio; P. O. Mazur; G. Medina-Tanco; M. Melissas; D. Melo; E. Menichetti; A. Menshikov; P. Mertsch; C. Meurer; S. Mi?anovi?; M. I. Micheletti; W. Miller; L. Miramonti; S. Mollerach; M. Monasor; D. Monnier Ragaigne; F. Montanet; B. Morales; C. Morello; E. Moreno; J. C. Moreno; C. Morris; M. Mostafá; C. A. Moura; S. Mueller; M. A. Muller; G. Müller; M. Münchmeyer; R. Mussa; G. Navarra; J. L. Navarro; S. Navas; P. Necesal; L. Nellen; A. Nelles; J. Neuser; P. T. Nhung; L. Niemietz; N. Nierstenhoefer; D. Nitz; D. Nosek; L. Nožka; M. Nyklicek; J. Oehlschläger; A. Olinto; V. M. Olmos-Gilbaja; M. Ortiz; N. Pacheco; D. Pakk Selmi-Dei; M. Palatka; J. Pallotta; N. Palmieri; G. Parente; E. Parizot; A. Parra; R. D. Parsons; S. Pastor; T. Paul; M. Pech; J. P?kala; R. Pelayo; I. M. Pepe; L. Perrone; R. Pesce; E. Petermann; S. Petrera; P. Petrinca; A. Petrolini; Y. Petrov; J. Petrovic; C. Pfendner; N. Phan; R. Piegaia; T. Pierog; P. Pieroni; M. Pimenta; V. Pirronello; M. Platino; V. H. Ponce; M. Pontz; P. Privitera; M. Prouza; E. J. Quel; S. Querchfeld; J. Rautenberg; O. Ravel; D. Ravignani; B. Revenu; J. Ridky; S. Riggi; M. Risse; P. Ristori; H. Rivera; V. Rizi; J. Roberts; C. Robledo; W. Rodrigues de Carvalho; G. Rodriguez; J. Rodriguez Martino; J. Rodriguez Rojo; I. Rodriguez-Cabo; M. D. Rodríguez-Frías; G. Ros; J. Rosado

2011-07-24T23:59:59.000Z

369

E-print Network : Main View : Search Results for Title: "Cosmic...  

Office of Scientific and Technical Information (OSTI)

Search: Title: "Cosmic Calibration" Did you mean ? Create new alert from this search New Search | My Selections (0) | | | | Alerts | Source Status Activity Indicator 0 top results...

370

ANL/ALCF/ESP-13/5 Cosmic Structure Probes of the Dark Universe  

NLE Websites -- All DOE Office Websites (Extended Search)

or any agency thereof, Argonne National Laboratory, or UChicago Argonne, LLC. ANLALCFESP-135 Cosmic Structure Probes of the Dark Universe (Porting and Tuning HACC on Mira)...

371

ASSESSING THE FEASIBILITY OF COSMIC-RAY ACCELERATION BY MAGNETIC TURBULENCE AT THE GALACTIC CENTER  

SciTech Connect

The presence of relativistic particles at the center of our Galaxy is evidenced by the diffuse TeV emission detected from the inner {approx}2 Degree-Sign of the Galaxy. Although it is not yet entirely clear whether the origin of the TeV photons is due to hadronic or leptonic interactions, the tight correlation of the intensity distribution with the distribution of molecular gas along the Galactic ridge strongly points to a pionic-decay process involving relativistic protons. In previous work, we concluded that point-source candidates, such as the supermassive black hole Sagittarius A* (identified with the High-Energy Stereoscopic System (HESS) source J1745-290) or the pulsar wind nebulae dispersed along the Galactic plane, could not account for the observed diffuse TeV emission from this region. Motivated by this result, we consider here the feasibility that the cosmic rays populating the Galactic center region are accelerated in situ by magnetic turbulence. Our results indicate that even in a highly conductive environment, this mechanism is efficient enough to energize protons within the intercloud medium to the {approx}>TeV energies required to produce the HESS emission.

Fatuzzo, M. [Physics Deparment, Xavier University, Cincinnati, OH 45207 (United States); Melia, F., E-mail: fatuzzo@xavier.edu, E-mail: fmelia@email.arizona.edu [Department of Physics, Applied Math Program, and Steward Observatory, University of Arizona, AZ 85721 (United States)

2012-05-01T23:59:59.000Z

372

DESPIKING OF SPACECRAFT ENERGETIC PROTON FLUX TO STUDY GALACTIC COSMIC-RAY MODULATION  

Science Conference Proceedings (OSTI)

Galactic cosmic ray (GCR) is usually assumed as a stable 'background', with solar influence considered as a modulation. The violent solar energetic particle (SEP) events associated with solar activities change particle fluxes by several orders of magnitude in a few minutes. Thus, the flux observation of GCR provided by satellites may be heavily contaminated by spurious spikes due to SEPs, and that provided by ground-based neutron monitors (NMs) may be contaminated by the system error spikes and the ground level enhancement effect. To obtain the 'pure' background GCR flux for modulation research, the removal of multifarious spikes is necessary. In this article, we use a robust automatic despiking algorithm based on the Poincare map thresholding method provided by Goring and Nikora for 'purification' of the time-series GCR flux observations. We can show that the algorithm is good at cleaning up the heavily contaminated GCR intensity rates measured by both spacecraft and NMs without artificial parameters. In addition, using the algorithm to despike the spacecraft observations of relatively lower energetic proton flux, we get both 11 year and 27 day period cycles comparable to the much higher energy GCR flux data measured by the ground-based NMs.

Qin, G.; Zhao, L.-L. [State Key Laboratory of Space Weather, Center for Space Science and Applied Research, Chinese Academy of Sciences, Beijing 100190 (China); Chen, H.-C., E-mail: gqin@spaceweather.ac.cn, E-mail: llzhao@spaceweather.ac.cn, E-mail: chchao@mail.ustc.edu.cn [Laboratory of Geophysical experiment, Institute of Geophysics, China Earthquake Administration, Beijing 100081 (China)

2012-06-20T23:59:59.000Z

373

EFFECTS OF NEUTRAL HYDROGEN ON COSMIC-RAY PRECURSORS IN SUPERNOVA REMNANT SHOCK WAVES  

Science Conference Proceedings (OSTI)

Many fast supernova remnant shocks show spectra dominated by Balmer lines. The H{alpha} profiles have a narrow component explained by direct excitations and a thermally Doppler broadened component due to atoms that undergo charge exchange in the post-shock region. However, the standard model does not take into account the cosmic-ray shock precursor, which compresses and accelerates plasma ahead of the shock. In strong precursors with sufficiently high densities, the processes of charge exchange, excitation, and ionization will affect the widths of both narrow and broad line components. Moreover, the difference in velocity between the neutrals and the precursor plasma gives rise to frictional heating due to charge exchange and ionization in the precursor. In extreme cases, all neutrals can be ionized by the precursor. In this Letter we compute the ion and electron heating for a wide range of shock parameters, along with the velocity distribution of the neutrals that reach the shock. Our calculations predict very large narrow component widths for some shocks with efficient acceleration, along with changes in the broad-to-narrow intensity ratio used as a diagnostic for the electron-ion temperature ratio. Balmer lines may therefore provide a unique diagnostic of precursor properties. We show that heating by neutrals in the precursor can account for the observed H{alpha} narrow component widths and that the acceleration efficiency is modest in most Balmer line shocks observed thus far.

Raymond, John C. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Vink, J.; Helder, E. A.; De Laat, A., E-mail: jraymond@cfa.harvard.edu [Astronomical Institute, Utrecht University, P.O. Box 80000, 3508TA Utrecht (Netherlands)

2011-04-10T23:59:59.000Z

374

U.S. Commercial Buildings Energy Intensity  

U.S. Energy Information Administration (EIA)

Glossary Home > Households, Buildings & Industry > Energy Efficiency > Commercial Buildings Energy Intensities > Table 5b

375

U.S. Commercial Buildings Energy Intensity  

U.S. Energy Information Administration (EIA)

Energy Efficiency > Commercial Buildings Energy Intensities > Table 6a. U.S. Commercial Buildings Energy

376

U.S. Commercial Buildings Energy Intensity  

U.S. Energy Information Administration (EIA)

Glossary Home > Households, Buildings & Industry > Energy Efficiency > Commercial Buildings Energy Intensities > Table 5a

377

U.S. Commercial Buildings Energy Intensity  

U.S. Energy Information Administration (EIA)

Glossary Home > Households, Buildings & Industry > Energy Efficiency > Commercial Buildings Energy Intensities > Table 7a

378

U.S. Commercial Buildings Energy Intensity  

U.S. Energy Information Administration (EIA)

Glossary Home > Households, Buildings & Industry > Energy Efficiency > Commercial Buildings Energy Intensities > Table7c

379

U.S. Commercial Buildings Energy Intensity  

U.S. Energy Information Administration (EIA)

Glossary Home > Households, Buildings & Industry > Energy Efficiency > Commercial Buildings Energy Intensities > Table 7b

380

Hierarchical Growth and Cosmic Star Formation: Enrichment, Outflows and Supernova Rates  

E-Print Network (OSTI)

The cosmic star formation histories are evaluated for different minimum masses of the initial halo structures, with allowance for realistic gas outflows. With a minimum halo mass of 10^{7} - 10^{8} M_odot and a moderate outflow efficiency, we reproduce both the current baryon fraction and the early chemical enrichment of the IGM. The intensity of the formation rate of ``normal'' stars is also well constrained by the observations: it has to be dominated by star formation in elliptical galaxies, except perhaps at very low redshift. The fraction of baryons in stars is predicted as are also the type Ia and II supernova event rates. Comparison with SN observations in the redshift range z=0-2 allows us to set strong constraints on the time delay of type Ia supernovae (a total delay of \\sim 4 Gyr is required to fit the data), the lower end of the mass range of the progenitors (2 - 8 M_odot) and the fraction of white dwarfs that reproduce the type Ia supernova (about 1 per cent). The intensity in the initial starburst of zero metallicity stars below 270 M_\\odot must be limited in order to avoid premature overenrichment of the IGM. Only about 10 - 20 % of the metals present in the IGM at z = 0 have been produced by population III stars at very high z. The remaining 80 - 90 % are ejected later by galaxies forming normal stars, with a maximum outflow efficiency occurring at a redshift of about 5. We conclude that 10^{-3} of the mass in baryons must lie in first massive stars in order to produce enough ionizing photons to allow early reionization of the IGM by z \\sim 15.

Frederic Daigne; Keith A. Olive; Joe Silk; Felix Stoehr; Elisabeth Vangioni

2005-09-07T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
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381

Search for the Cosmic Neutrino Background and KATRIN  

E-Print Network (OSTI)

The Cosmic Microwave Background (CMB) has been detected in 1964 by Penzias and Wilson. It shows today a remarkable constant temperature of T ~ 2.7 K independent of the direction. Present density is about 370 photons per cubic-cm. The size of the hot spots, which deviates only in the fifth decimal of the temperature from the average value, tells us, that the universe is flat. About 300 000 years after the Big Bang at a temperature of T = 3000 K already in the matter dominated era the electrons combine with the protons and 4He and the photons move freely in the neutral universe. So the temperature and distribution of the photons give us information of the universe 300 000 years after the Big Bang. Information about earlier times can, in principle, be derived from the Cosmic Neutrino Background. The neutrinos decouple already 1 second after the Big Bang at a temperature of about 10^{10} K. Today their temperature is ~ 1.95 K and the average density is 56 electron-neutrinos per cubic-cm. Registration of these neutrinos is an extremely challenging experimental problem which can hardly be solved with the present technologies. On the other hand it represents a tempting opportunity to check one of the key element of the Big Bang cosmology and to probe the early stages of the universe evolution. The search for the cosmic relic neutrinos with the induced beta decay Electron-neutrino + 3H --> 3He + e- is the topic of this contribution. The signal would show up by a peak in the electron spectrum with an energy of the neutrino mass above the Q value. We discuss the prospects of this approach and argue that it is able to set limits on the relic neutrino density in our vicinity.

Amand Faessler; Rastislav Hodak; Sergey Kovalenko; Fedor Simkovic

2013-04-20T23:59:59.000Z

382

Dark matter searches with cosmic antideuterons: status and perspectives  

E-Print Network (OSTI)

The search for antideuterons in cosmic rays has been proposed as a promising channel for dark matter indirect detection, especially for dark matter particles with a low or intermediate mass. With the current operational phase of the AMS-02 experiment and the ongoing development of a future dedicated experiment, the General Antiparticle Spectrometer (GAPS), there are exciting prospects for a dark matter detection in the near future. In this paper we develop a detailed and complete re-analysis of the cosmic-ray antideuteron signal, by discussing the main relevant issues related to antideuteron production and propagation through the interstellar medium and the heliosphere. In particular, we first critically revisit the coalescence mechanism for antideuteron production in dark matter annihilation processes. Then, since antideuteron searches have their best prospects of detection at low kinetic energies where the effect of the solar wind and magnetic field are most relevant, we address the impact of solar modulation modeling on the antideuteron flux at the Earth by developing a full numerical 4D solution of cosmic rays transport in the heliosphere. We finally use these improved predictions to provide updated estimates of the reaching capabilities for AMS-02 and GAPS, compatible with the current constraints imposed by the antiprotons measurements of PAMELA. After the antiproton bound is applied, prospects of detection of up to about 15 events in GAPS LDB+ and AMS-02 missions are found, depending on the dark matter mass, annihilation rate and production channel from one side, and on the coalescence process, galactic and solar transport parameters on the other.

N. Fornengo; L. Maccione; A. Vittino

2013-06-18T23:59:59.000Z

383

TRACING THE SOURCES OF COSMIC RAYS WITH MOLECULAR IONS  

Science Conference Proceedings (OSTI)

The rate of ionization by cosmic rays (CRs) in interstellar gas directly associated with {gamma}-ray-emitting supernova remnants (SNRs) is for the first time calculated to be several orders of magnitude larger than the Galactic average. Analysis of ionization-induced chemistry yields the first quantitative prediction of the astrophysical H{sup +} {sub 2} emission line spectrum, which should be detectable together with H{sup +} {sub 3} lines. The predicted coincident observation of those emission lines and {gamma}-rays will help prove that SNRs are sources of CRs.

Becker, Julia K.; Schuppan, Florian [Ruhr-Universitaet Bochum, Fakultaet fuer Physik and Astronomie, Theoretische Physik IV, D-44780 Bochum (Germany); Black, John H.; Mohammadtaher Safarzadeh, E-mail: julia@tp4.rub.de [Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, SE-439 92 Onsala (Sweden)

2011-10-01T23:59:59.000Z

384

The Composition of Cosmic Rays at the Knee  

E-Print Network (OSTI)

The observation of a small change in spectral slope, or ’knee ’ in the fluxes of cosmic rays near energies 10 15 eV has caused much speculation since its discovery over 40 years ago. The origin of this feature remains unknown. A small workshop to review some modern experimental measurements of this region was held at the Adler Planetarium in Chicago, USA in June 2000. This paper summarizes the results presented at this workshop and the discussion of their interpretation in the context of hadronic models of atmospheric airshowers.

S. P. Swordy; L. F. Fortson; El A; C. L. Pryke; T. Shibata; S. P. Wakely; Z. Cao; M. L. Cherry; S. Coutu; J. Cronin; R. Engel; J. W. Fowler; S. A. Minnick; A. Moiseev; D. Muller; M. Roth; A. Sill; G. Spiczak H

2002-01-01T23:59:59.000Z

385

The Composition of Cosmic Rays at the Knee  

E-Print Network (OSTI)

The observation of a small change in spectral slope, or 'knee' in the fluxes of cosmic rays near energies 10^15 eV has caused much speculation since its discovery over 40 years ago. The origin of this feature remains unknown. A small workshop to review some modern experimental measurements of this region was held at the Adler Planetarium in Chicago, USA in June 2000. This paper summarizes the results presented at this workshop and the discussion of their interpretation in the context of hadronic models of atmospheric airshowers.

S. P. Swordy; L. F. Fortson; J. Hinton; J. Horandel; J. Knapp; C. L. Pryke; T. Shibata; S. P. Wakely; Z. Cao; M. L. Cherry; S. Coutu; J. Cronin; R. Engel; J. W. Fowler; K. - H. Kampert; J. Kettler; D. B. Kieda; J. Matthews; S. A. Minnick; A. Moiseev; D. Muller; M. Roth; A. Sill; G. Spiczak

2002-02-07T23:59:59.000Z

386

Cosmic Ray Positrons at High Energies: A New Measurement  

E-Print Network (OSTI)

We present a new measurement of the cosmic-ray positron fraction e+/(e+ + e-) obtained from the first balloon flight of the High Energy Antimatter Telescope (HEAT). Using a magnet spectrometer combined with a transition radiation detector, an electromagnetic calorimeter, and time-of-flight counters we have achieved a high degree of background rejection. Our results do not indicate a major contribution to the positron flux from primary sources. In particular, we see no evidence for the significant rise in the positron fraction at energies above ~10 GeV previously reported.

HEAT Collaboration

1995-05-30T23:59:59.000Z

387

Gamma-Ray Bursts and Quantum Cosmic Censorship  

E-Print Network (OSTI)

Gamma-ray bursts are believed to result from the coalescence of binary neutron stars. However, the standard proposals for conversion of the gravitational energy to thermal energy have difficulties. We show that if the merger of the two neutron stars results in a naked singularity, instead of a black hole, the ensuing quantum particle creation can provide the requisite thermal energy in a straightforward way. The back-reaction of the created particles can avoid the formation of the naked singularity predicted by the classical theory. Hence cosmic censorship holds in the quantum theory, even if it were to be violated in classical general relativity.

T. P. Singh

1998-05-17T23:59:59.000Z

388

Cerenkov radiation from collisions of straight cosmic (super)strings  

E-Print Network (OSTI)

We consider Cerenkov radiation which must arise when randomly oriented straight cosmic (super)strings move with relativistic velocities without intercommutation. String interactions via dilaton, two-form and gravity (gravity being the dominant force in the ultra-relativistic regime) leads to formation of superluminal sources which generate Cerenkov radiation of dilatons and axions. Though the effect is of the second order in the couplings of strings to these fields, its total efficiency is increased by high dependence of the radiation rate on the Lorentz-factor of the collision.

Elena Melkumova; Dmitri Gal'tsov; Karim Salehi

2006-12-26T23:59:59.000Z

389

Bosonic (meta)stabilization of cosmic string loops  

E-Print Network (OSTI)

We consider the possibility of a bosonic (meta)stabilization of a cosmic gauge string loop due to the presence of a gas of low mass bosonic particles which become trapped within the string core. This boson gas exerts a pressure which tends to counteract the string tension, allowing a circular string loop to find a finite equilibrium radius, provided that gas particles do not escape the string core. However, high energy bosons do escape, and consequently the loop shrinks and the temperature rises. Estimates indicate that the bosonic stabilization mechanism is ineffective, and the loop is unstable against decay.

J. R. Morris

2013-03-08T23:59:59.000Z

390

Forecasting Cosmic Doomsday from CMB/LSS Cross-Correlations  

E-Print Network (OSTI)

A broad class of dark energy models, which have been proposed in attempts at solving the cosmological constant problems, predict a late time variation of the equation of state with redshift. The variation occurs as a scalar field picks up speed on its way to negative values of the potential. The negative potential energy eventually turns the expansion into contraction and the local universe undergoes a big crunch. In this paper we show that cross-correlations of the CMB anisotropy and matter distribution, in combination with other cosmological data, can be used to forecast the imminence of such cosmic doomsday.

Jaume Garriga; Levon Pogosian; Tanmay Vachaspati

2003-11-17T23:59:59.000Z

391

Assessing the Impact of Simulated COSMIC GPS Radio Occultation Data on Weather Analysis over the Antarctic: A Case Study  

Science Conference Proceedings (OSTI)

The Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC) mission was launched in April 2006. As part of its mission, COSMIC will provide approximately 2500–3000 global positioning system (GPS) radio occultation (RO) ...

L. Cucurull; Y-H. Kuo; D. Barker; S. R. H. Rizvi

2006-11-01T23:59:59.000Z

392

The Effect of Atmospheric Water Vapor on Neutron Count in the Cosmic-Ray Soil Moisture Observing System  

Science Conference Proceedings (OSTI)

The cosmic-ray method for measuring soil moisture, used in the COsmic-ray Soil Moisture Observing System (COSMOS), relies on the exceptional ability of hydrogen to moderate fast neutrons. Sources of hydrogen near the ground, other than soil ...

R. Rosolem; W. J. Shuttleworth; M. Zreda; T. E. Franz; X. Zeng; S. A. Kurc

393

The Effect of Atmospheric Water Vapor on Neutron Count in the Cosmic-Ray Soil Moisture Observing System  

Science Conference Proceedings (OSTI)

The cosmic-ray method for measuring soil moisture, used in the Cosmic-Ray Soil Moisture Observing System (COSMOS), relies on the exceptional ability of hydrogen to moderate fast neutrons. Sources of hydrogen near the ground, other than soil ...

R. Rosolem; W. J. Shuttleworth; M. Zreda; T. E. Franz; X. Zeng; S. A. Kurc

2013-10-01T23:59:59.000Z

394

Ultra High Energy Particles Propagation and the Transition from Galactic to Extra-Galactic Cosmic Rays  

E-Print Network (OSTI)

We discuss the basic features of the propagation of Ultra High Energy Cosmic Rays in astrophysical backgrounds, comparing two alternative computation schemes to compute the expected fluxes. We also discuss the issue of the transition among galactic and extra-galactic cosmic rays using theoretical results on fluxes to compare different models.

Aloisio, Roberto

2013-01-01T23:59:59.000Z

395

Convertibility of Function Points into COSMIC Function Points: A study using Piecewise Linear Regression  

Science Conference Proceedings (OSTI)

Background: COSMIC Function Points and traditional Function Points (i.e., IFPUG Function Points and more recent variation of Function Points, such as NESMA and FISMA) are probably the best known and most widely used Functional Size Measurement methods. ... Keywords: COSMIC Function Points, Data analysis, Function Point analysis, Functional Size Measurement, Functional size measure convertibility, Outliers

Luigi Lavazza; Sandro Morasca

2011-08-01T23:59:59.000Z

396

Are extragalactic gamma ray bursts the source of the highest energy cosmic rays?  

E-Print Network (OSTI)

Recent observations with the large air shower arrays of ultra high energy cosmic rays (UHECR) and recent measurements/estimates of the redshifts of gamma ray bursts (GRBs) seem to rule out extragalactic GRBs as the source of the cosmic rays that are observed near Earth, including those with the highest energies.

Arnon Dar

1999-01-03T23:59:59.000Z

397

Star Wars Forever? --A Cosmic Perspective Joel R. Primack and Nancy Ellen Abrams  

E-Print Network (OSTI)

changes in the entire Earth, when we view the present epoch in the history of our planet in cosmic are helping us to understand the history of our own cosmic home, the Milky Way galaxy.4 In the seventeenth Hussein, who set fire to the oil wells in Kuwait and caused an environmental disaster with no military

California at Santa Cruz, University of

398

The rise and fall of cosmical physics: notes for a history, ca. 1850-1920  

E-Print Network (OSTI)

In the period from about 1890 to 1915 an interdisciplinary and unifying research programme known as "cosmical physics" attracted much scientific and public attention. It typically included aspects of the earth sciences (such as magnetic storms and atmospheric electricity) combined with astronomical subjects (such as the solar corona and cometary tails), but there was no unanimity as to the precise meaning of cosmical physics, which collapsed after World War I. The essay covers the history of cosmical physics as it unfolded in particular in Germany, Austria, England and Scandinavia. Among the scientists who contributed to the development of cosmical physics were Wilhelm Foerster from Germany, Wilhelm Trabert from Austria, Kristian Birkeland from Norway and Svante Arrhenius from Sweden. While cosmical physics did not usually involve a cosmological dimension, both Birkeland and Arrhenius constructed cosmologies based on their work on auroral and other phenomena.

Kragh, Helge

2013-01-01T23:59:59.000Z

399

Forecast constraints on cosmic string parameters from gravitational wave direct detection experiments  

E-Print Network (OSTI)

Gravitational waves (GWs) are one of the key signatures of cosmic strings. If GWs from cosmic strings are detected in future experiments, not only their existence can be confirmed but also their properties might be probed. In this paper, we study the determination of cosmic string parameters through direct detection of GW signatures in future ground-based GW experiments. We consider two types of GWs, bursts and the stochastic GW background, which provide us with different information about cosmic string properties. Performing the Fisher matrix calculation on the cosmic string parameters, such as parameters governing the string tension $G\\mu$ and initial loop size $\\alpha$ and the reconnection probability $p$, we find that the two different types of GW can break degeneracies in some of these parameters and provide better constraints than those from each measurement.

Sachiko Kuroyanagi; Koichi Miyamoto; Toyokazu Sekiguchi; Keitaro Takahashi; Joseph Silk

2012-02-14T23:59:59.000Z

400

Efficiency of Nonlinear Particle Acceleration at Cosmic Structure Shocks  

E-Print Network (OSTI)

We have calculated the evolution of cosmic ray (CR) modified astrophysical shocks for a wide range of shock Mach numbers and shock speeds through numerical simulations of diffusive shock acceleration (DSA) in 1D quasi- parallel plane shocks. The simulations include thermal leakage injection of seed CRs, as well as pre-existing, upstream CR populations. Bohm-like diffusion is assumed. We model shocks similar to those expected around cosmic structure pancakes as well as other accretion shocks driven by flows with upstream gas temperatures in the range $T_0=10^4-10^{7.6}$K and shock Mach numbers spanning $M_s=2.4-133$. We show that CR modified shocks evolve to time-asymptotic states by the time injected particles are accelerated to moderately relativistic energies ($p/mc \\gsim 1$), and that two shocks with the same Mach number, but with different shock speeds, evolve qualitatively similarly when the results are presented in terms of a characteristic diffusion length and diffusion time. For these models the time asymptotic value for the CR acceleration efficiency is controlled mainly by shock Mach number. The modeled high Mach number shocks all evolve towards efficiencies $\\sim 50$%, regardless of the upstream CR pressure. On the other hand, the upstream CR pressure increases the overall CR energy in moderate strength shocks ($M_s \\sim {\\rm a few}$). (abridged)

H. Kang; T. W. Jones

2004-10-29T23:59:59.000Z

Note: This page contains sample records for the topic "intensity frontier cosmic" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


401

GZK Photons as Ultra High Energy Cosmic Rays  

E-Print Network (OSTI)

We calculate the flux of "GZK-photons", namely the flux of Ultra High Energy Cosmic Rays (UHECR) consisting of photons produced by extragalactic nucleons through the resonant photoproduction of pions, the so called GZK effect. We We calculate the flux of "GZK-photons", namely the flux of Ultra High Energy Cosmic Rays (UHECR) consisting of photons produced by extragalactic nucleons through the resonant photoproduction of pions, the so called GZK effect. We show that, for primary nucleons, the GZK photon fraction of the total UHECR flux is between $10^{-4}$ and $10^{-2}$ above $10^{19}$ eV and up to the order of 0.1 above $10^{20}$ eV. The GZK photon flux depends on the assumed UHECR spectrum, slope of the nucleon flux at the source, distribution of sources and intervening backgrounds. Detection of this photon flux would open the way for UHECR gamma-ray astronomy. Detection of a larger photon flux would imply the emission of photons at the source or new physics. We compare the photon fractions expected for GZK photons and the minimal predicted by Top-Down models. We find that the photon fraction above $10^{19}$ eV is a crucial test for Top-Down models.

Graciela B. Gelmini; Oleg E. Kalashev; Dmitry V. Semikoz

2005-06-06T23:59:59.000Z

402

Duality relation between radiation thermodynamics and cosmic string loop thermodynamics  

SciTech Connect

We discuss thermodynamics of electromagnetic radiation, with p=(1/3){rho} and S{proportional_to}T{sup 3}V, and of cosmic string loops, with p=-(1/3){rho} and S{proportional_to}T{sup -3}V, where p stands for pressure, T temperature, {rho} energy density, S entropy, and V volume. We write the thermodynamic formalisms under a common framework that illustrates their formal relationship and allows us to go from one to the other through a smooth transformation. From a microscopic perspective, these relations arise from the energy relations u({lambda})=hc/{lambda} for the photons of electromagnetic radiation, and u(l)=(c{sup 4}/a{sup 2}G)l for cosmic string loops, a being a numerical (dimensionless) constant and {lambda} and l the radiation wavelength and the length of a loop; G, c, and h are the gravitational constant, the speed of light in vacuo, and the Planck constant, respectively. The corresponding thermodynamic behaviors are seen to be connected through a related thermal duality corresponding to the change of T by T*=T{sub c}{sup 2}/T, with T{sub c} a reference temperature related to h, c, and G.

Jou, D. [Departament de Fisica, Universitat Autonoma de Barcelona, 08193 Bellaterra, Catalonia (Spain); Mongiovi, M. S. [Dipartimento di Metodi e Modelli Matematici, Universita di Palermo, 90128 Palermo (Italy); Sciacca, M. [Dipartimento di Sistemi Agro-Ambientali, Universita di Palermo, 90128 Palermo (Italy)

2011-05-15T23:59:59.000Z

403

THE DISCOVERY OF GEOMAGNETICALLY TRAPPED COSMIC-RAY ANTIPROTONS  

Science Conference Proceedings (OSTI)

The existence of a significant flux of antiprotons confined to Earth's magnetosphere has been considered in several theoretical works. These antiparticles are produced in nuclear interactions of energetic cosmic rays with the terrestrial atmosphere and accumulate in the geomagnetic field at altitudes of several hundred kilometers. A contribution from the decay of albedo antineutrons has been hypothesized in analogy to proton production by neutron decay, which constitutes the main source of trapped protons at energies above some tens of MeV. This Letter reports the discovery of an antiproton radiation belt around the Earth. The trapped antiproton energy spectrum in the South Atlantic Anomaly (SAA) region has been measured by the PAMELA experiment for the kinetic energy range 60-750 MeV. A measurement of the atmospheric sub-cutoff antiproton spectrum outside the radiation belts is also reported. PAMELA data show that the magnetospheric antiproton flux in the SAA exceeds the cosmic-ray antiproton flux by three orders of magnitude at the present solar minimum, and exceeds the sub-cutoff antiproton flux outside radiation belts by four orders of magnitude, constituting the most abundant source of antiprotons near the Earth.

Adriani, O. [Department of Physics, University of Florence, I-50019 Sesto Fiorentino, Florence (Italy); Barbarino, G. C. [Department of Physics, University of Naples 'Federico II', I-80126 Naples (Italy); Bazilevskaya, G. A. [Lebedev Physical Institute, RU-119991, Moscow (Russian Federation); Bellotti, R.; Bruno, A.; Cafagna, F. [Department of Physics, University of Bari, I-70126 Bari (Italy); Boezio, M.; Bonvicini, V. [INFN, Sezione di Trieste, I-34149 Trieste (Italy); Bogomolov, E. A. [Ioffe Physical Technical Institute, RU-194021 St. Petersburg (Russian Federation); Bongi, M.; Bottai, S. [INFN, Sezione di Florence, I-50019 Sesto Fiorentino, Florence (Italy); Borisov, S.; Casolino, M.; De Pascale, M. P.; De Santis, C. [INFN, Sezione di Rome 'Tor Vergata', I-00133 Rome (Italy); Campana, D.; Carbone, R.; Consiglio, L. [INFN, Sezione di Naples, I-80126 Naples (Italy); Carlson, P. [KTH, Department of Physics, and the Oskar Klein Centre for Cosmoparticle Physics, AlbaNova University Centre, SE-10691 Stockholm (Sweden); Castellini, G., E-mail: alessandro.bruno@ba.infn.it [IFAC, I-50019 Sesto Fiorentino, Florence (Italy)

2011-08-20T23:59:59.000Z

404

The discovery of geomagnetically trapped cosmic ray antiprotons  

E-Print Network (OSTI)

The existence of a significant flux of antiprotons confined to Earth's magnetosphere has been considered in several theoretical works. These antiparticles are produced in nuclear interactions of energetic cosmic rays with the terrestrial atmosphere and accumulate in the geomagnetic field at altitudes of several hundred kilometers. A contribution from the decay of albedo antineutrons has been hypothesized in analogy to proton production by neutron decay, which constitutes the main source of trapped protons at energies above some tens of MeV. This Letter reports the discovery of an antiproton radiation belt around the Earth. The trapped antiproton energy spectrum in the South Atlantic Anomaly (SAA) region has been measured by the PAMELA experiment for the kinetic energy range 60--750 MeV. A measurement of the atmospheric sub-cutoff antiproton spectrum outside the radiation belts is also reported. PAMELA data show that the magnetospheric antiproton flux in the SAA exceeds the cosmic-ray antiproton flux by three orders of magnitude at the present solar minimum, and exceeds the sub-cutoff antiproton flux outside radiation belts by four orders of magnitude, constituting the most abundant source of antiprotons near the Earth.

O. Adriani; G. C. Barbarino; G. A. Bazilevskaya; R. Bellotti; M. Boezio; E. A. Bogomolov; M. Bongi; V. Bonvicini; S. Borisov; S. Bottai; A. Bruno; F. Cafagna; D. Campana; R. Carbone; P. Carlson; M. Casolino; G. Castellini; L. Consiglio; M. P. De Pascale; C. De Santis; N. De Simone; V. Di Felice; A. M. Galper; W. Gillard; L. Grishantseva; G. Jerse; A. V. Karelin; M. D. Kheymits; S. V. Koldashov; S. Y. Krutkov; A. N. Kvashnin; A. Leonov; V. Malakhov; L. Marcelli; A. G. Mayorov; W. Menn; V. V. Mikhailov; E. Mocchiutti; A. Monaco; N. Mori; N. Nikonov; G. Osteria; F. Palma; P. Papini; M. Pearce; P. Picozza; C. Pizzolotto; M. Ricci; S. B. Ricciarini; L. Rossetto; R. Sarkar; M. Simon; R. Sparvoli; P. Spillantini; Y. I. Stozhkov; A. Vacchi; E. Vannuccini; G. Vasilyev; S. A. Voronov; Y. T. Yurkin; J. Wu; G. Zampa; N. Zampa; V. G. Zverev

2011-07-25T23:59:59.000Z

405

Cosmic Solenoids: Minimal Cross-Section and Generalized Flux Quantization  

E-Print Network (OSTI)

A self-consistent general relativistic configuration describing a finite cross-section magnetic flux tube is constructed. The cosmic solenoid is modeled by an elastic superconductive surface which separates the Melvin core from the surrounding flat conic structure. We show that a given amount $\\Phi$ of magnetic flux cannot be confined within a cosmic solenoid of circumferential radius smaller than $\\frac{\\sqrt{3G}}{2\\pi c^2}\\Phi$ without creating a conic singularity. Gauss-Codazzi matching conditions are derived by means of a self-consistent action. The source term, representing the surface currents, is sandwiched between internal and external gravitational surface terms. Surface superconductivity is realized by means of a Higgs scalar minimally coupled to projective electromagnetism. Trading the 'magnetic' London phase for a dual 'electric' surface vector potential, the generalized quantization condition reads: $e/{hc} \\Phi + 1/e Q=n$ with $Q$ denoting some dual 'electric' charge, thereby allowing for a non-trivial Aharonov-Bohm effect. Our conclusions persist for dilaton gravity provided the dilaton coupling is sub-critical.

Aharon Davidson; David Karasik

1999-01-02T23:59:59.000Z

406

Cosmic String constraints from WMAP and the South Pole Telescope  

E-Print Network (OSTI)

The predictions of the inflationary LCDM paradigm match today's high-precision measurements of the cosmic microwave background anisotropy extremely well. The same data put tight limits on other sources of anisotropy. Cosmic strings are a particularly interesting alternate source to constrain. Strings are topological defects, remnants of inflationary-era physics that persist after the big bang. They are formed in a variety of models of inflation, including string theory models such as brane inflation. We assume a "Nambu-Goto" model for strings, approximated by a collection of unconnected segments with zero width, and show that measurements of temperature anisotropy by the South Pole Telescope break a parameter degeneracy in the WMAP data, permitting us to place a strong upper limit on the possible string contribution to the CMB anisotropy: the power sourced by zero-width strings must be <1.75% (95% CL) of the total or the string tension Gmu <1.7x10^{-7}. These limits imply that the best hope for detecting strings in the CMB will come from B-mode polarization measurements at arcminute scales rather than the degree scale measurements pursued for gravitational wave detection.

Cora Dvorkin; Mark Wyman; Wayne Hu

2011-09-22T23:59:59.000Z

407

Enhanced oil recovery utilizing high-angle wells in the Frontier Formation, Badger Basin Field, Park County, Wyoming. Final report for the period October 1992--October 1993  

SciTech Connect

Badger Basin Field, discovered in 1931, produces at stripper rates from low-permeability fractured sandstones of the Upper Cretaceous Frontier Formation. Only 15% of the estimated 25 million barrels of oil originally in-place will be produced from the twenty-two attempted vertical completions. This project will increase recoverable reserves through a better understanding of the reservoir and factors which control production. Characterization of the reservoir has been accomplished through an integrated engineering, geological and geophysical approach. Production data, drilling and completion techniques, and relative location of wells on the anticline were reviewed and related to productivity. Literature was reviewed for interpretations on preferred flow directions on anticlinal structures. A structure map of the producing Frontier reservoir was constructed. Porosity development and its relationship to fracture networks was examined petrographically. Fractures in core were described and oriented using paleomagnetic techniques. Azimuths of fractures in outcrop were compared to fracture azimuths measured in the core. A 17 square-mile 3D seismic survey was designed, acquired and processed. Interpretation is being performed on a Sun workstation using Landmark Graphics software. Time-structure and amplitude-distribution maps will be constructed on three Frontier horizons. A location for a high-angle well will be chosen. The slant/horizontal test will be drilled and completed to increase recovery of reserves. Transfer of successful technologies will be accomplished by technical publications and presentations, and access to project materials, data, and field facilities.

Walker, J.P.; Fortmann, R.G.

1994-12-01T23:59:59.000Z

408

On inconsistency of experimental data on primary nuclei spectra with sea level muon intensity measurements  

E-Print Network (OSTI)

For the first time a complete set of the most recent direct data on primary cosmic ray spectra is used as input into calculations of muon flux at sea level in wide energy range $E_\\mu=1-3\\cdot10^5$ GeV. Computations have been performed with the CORSIKA/QGSJET and CORSIKA/VENUS codes. The comparison of the obtained muon intensity with the data of muon experiments shows, that measurements of primary nuclei spectra conform to sea level muon data only up to several tens of GeV and result in essential deficit of muons at higher energies. As it follows from our examination, uncertainties in muon flux measurements and in the description of nuclear cascades development are not suitable to explain this contradiction, and the only remaining factor, leading to this situation, is underestimation of primary light nuclei fluxes. We have considered systematic effects, that may distort the results of the primary cosmic ray measurements with the application of the emulsion chambers. We suggest, that re-examination of these measurements is required with the employment of different hadronic interaction models. Also, in our point of view, it is necessary to perform estimates of possible influence of the fact, that sizable fraction of events, identified as protons, actually are antiprotons. Study of these cosmic ray component begins to attract much attention, but today nothing definite is known for the energies $>40$ GeV. In any case, to realize whether the mentioned, or some other reasons are the sources of disagreement of the data on primaries with the data on muons, the indicated effects should be thoroughly analyzed.

A. A. Lagutin; A. G. Tyumentsev; A. V. Yushkov

2004-02-06T23:59:59.000Z

409

Iron and Steel Energy Intensities  

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

If you are having trouble, call 202-586-8800 for help. Home > >Energy Users > Energy Efficiency Page > Iron and Steel Energy Intensities First Use of Energy Blue Bullet First Use/Value of Production Blue Bullet First Use/Ton of steel End Uses of Consumption Blue Bullet Total End Use/Value of Production Blue Bullet Total End Use/Ton of Steel Boiler Fuel as End Use Blue Bullet Boiler Fuel /Value of Production Blue Bullet Boiler Fuel /Ton of Steel Process Heating as End Use Blue Bullet Process Heating Fuel /Ton of Steel Blue Bullet Process Heating /Value of Production Machine Drive as End Use Blue Bullet Machine Drive Fuel/Ton of Steel Blue Bullet Machine Drive Fuel /Value of Production Expenditures Blue Bullet Purchased Fuel /Ton of Steel Blue Bullet Purchased Fuel /Value of Production

410

A novel multi-scale intensity metric for evaluation of tropical cyclone intensity forecasts  

Science Conference Proceedings (OSTI)

In this study, a new Multi-Scale Intensity (MSI) metric for evaluating Tropical Cyclone (TC) intensity forecasts is presented. The metric consists of the resolvable and observable, low wavenumber intensity represented by the sum of amplitudes of ...

Tomislava Vukicevic; Eric Uhlhorn; Paul Reasor; Bradley Klotz

411

Higher Hydroclimatic Intensity with Global Warming  

Science Conference Proceedings (OSTI)

Because of their dependence on water, natural and human systems are highly sensitive to changes in the hydrologic cycle. The authors introduce a new measure of hydroclimatic intensity (HY-INT), which integrates metrics of precipitation intensity ...

F. Giorgi; E.-S. Im; E. Coppola; N. S. Diffenbaugh; X. J. Gao; L. Mariotti; Y. Shi

2011-10-01T23:59:59.000Z

412

Environmental Control of Tropical Cyclone Intensity  

Science Conference Proceedings (OSTI)

The influence of various environmental factors on tropical cyclone intensity is explored using a simple coupled ocean–atmosphere model. It is first demonstrated that this model is capable of accurately replicating the intensity evolution of ...

Kerry Emanuel; Christopher DesAutels; Christopher Holloway; Robert Korty

2004-04-01T23:59:59.000Z

413

STABILIZED HIGH INTENSITY SOURCE OF 80 kv  

SciTech Connect

With the change of the current load from 0 to 2.5 mamp and simultaneous change of incoming intensity from 270 to 190 v, the stabilized high-intensity source changes less than l%.. The stabilized intensity can be arranged in steps of 5 kv from 60 to 80 kv. The high-intensity stabilizer automatically switches on upon reaching 60 kv. (tr-auth)

Polivanov, V.V.; Izyurov, A.V.; Pyatakov, N.I.

1959-09-01T23:59:59.000Z

414

Analytical theory of intensity fluctuations in SASE  

SciTech Connect

Recent advances in SASE experiments stimulate interest in quantitative comparison of measurements with theory. Extending the previous analysis of the SASE intensity in guided modes, the authors provide an analytical description of the intensity fluctuations by calculating intensity correlation functions in the frequency domain. Comparison of the results with experiment yields new insight into the SASE process.

Yu, L.H.; Krinsky, S. [Brookhaven National Lab., Upton, NY (United States). National Synchrotron Light Source

1997-07-01T23:59:59.000Z

415

Final Report to the Department of Energy on the 1994 International Accelerator School: Frontiers of Accelerator Technology  

SciTech Connect

The international accelerator school on Frontiers of Accelerator Technology was organized jointly by the US Particle Accelerator School (Dr. Mel Month and Ms. Marilyn Paul), the CERN Accelerator School, and the KEK Accelerator School, and was hosted by the University of Hawaii. The course was held on Maui, Hawaii, November 3-9, 1994 and was made possible in part by a grant from the Department of Energy under award number DE-FG03-94ER40875, AMDT M006. The 1994 program was preceded by similar joint efforts held at Santa Margherita di Pula, Sardinia in February 1985, South Padre Island, Texas in October 1986, Anacapri, Italy in October 1988, Hilton Head Island, South Carolina in October 1990, and Benalmedena, Spain in October/November 1992. The most recent program was held in Montreux, Switzerland in May 1998. The purpose of the program is to disseminate knowledge on the latest ideas and developments in the technology of particle accelerators by bringing together known world experts and younger scientists in the field. It is intended for individuals with professional interest in accelerator physics and technology, for graduate students, for post-docs, for those interested in accelerator based sciences, and for scientific and engineering staff at industrial firms, especially those companies specializing in accelerator components.

Harris, F.A.

1998-09-17T23:59:59.000Z

416

Energy Frontier Research Centers: Helping Win the Energy Innovation Race (2011 EFRC Summit Keynote Address, Secretary of Energy Chu)  

Science Conference Proceedings (OSTI)

Secretary of Energy Steven Chu gave the keynote address at the 2011 EFRC Summit and Forum. In his talk, Secretary Chu highlighted the need to "unleash America's science and research community" to achieve energy breakthroughs. The 2011 EFRC Summit and Forum brought together the EFRC community and science and policy leaders from universities, national laboratories, industry and government to discuss "Science for our Nation's Energy Future." In August 2009, the Office of Science established 46 Energy Frontier Research Centers. The EFRCs are collaborative research efforts intended to accelerate high-risk, high-reward fundamental research, the scientific basis for transformative energy technologies of the future. These Centers involve universities, national laboratories, nonprofit organizations, and for-profit firms, singly or in partnerships, selected by scientific peer review. They are funded at $2 to $5 million per year for a total planned DOE commitment of $777 million over the initial five-year award period, pending Congressional appropriations. These integrated, multi-investigator Centers are conducting fundamental research focusing on one or more of several “grand challenges” and use-inspired “basic research needs” recently identified in major strategic planning efforts by the scientific community. The purpose of the EFRCs is to integrate the talents and expertise of leading scientists in a setting designed to accelerate research that transforms the future of energy and the environment.

Chu, Steven (DOE Secretary of Energy)

2011-05-25T23:59:59.000Z

417

Detection of cosmic superstrings by geodesic test particle motion  

Science Conference Proceedings (OSTI)

(p,q)-strings are bound states of p F-strings and q D-strings and are predicted to form at the end of brane inflation. As such, these cosmic superstrings should be detectable in the Universe. In this paper we argue that they can be detected by the way that massive and massless test particles move in the space-time of these cosmic superstrings. In particular, we study solutions to the geodesic equation in the space-time of field theoretical (p,q)-strings. The geodesics can be classified according to the test particles' energy, angular momentum and momentum in the direction of the string axis. We discuss how the change of the magnetic fluxes, the ratio between the symmetry-breaking scale and the Planck mass, the Higgs-to-gauge-boson mass ratios and the binding between the F- and D-strings, respectively, influence the motion of the test particles. While massless test particles can move only on escape orbits, a new feature as compared to the infinitely thin string limit is the existence of bound orbits for massive test particles. In particular, we observe that--in contrast to the space-time of a single Abelian-Higgs string--bound orbits for massive test particles in (p,q)-string space-times are possible if the Higgs boson mass is larger than the gauge boson mass. We also compute the effect of the binding between the p- and the q-string on observables such as the light deflection and the perihelion shift. While light deflection can also be caused by other matter distributions, the possibility of a negative perihelion shift seems to be a feature of finite width cosmic strings that could lead to the unmistakable identification of such objects. In Melvin space-times, which are asymptotically nonconical, massive test particles have to move on bound orbits, while massless test particles can escape to infinity only if their angular momentum vanishes.

Hartmann, Betti; Sirimachan, Parinya [School of Engineering and Science, Jacobs University Bremen, 28759 Bremen (Germany); Laemmerzahl, Claus [ZARM, Universitaet Bremen, Am Fallturm, 28359 Bremen (Germany); Institut fuer Physik, Universitaet Oldenburg, 26111 Oldenburg (Germany)

2011-02-15T23:59:59.000Z

418

Are gamma-ray bursts the sources of ultra-high energy cosmic rays?  

E-Print Network (OSTI)

We reconsider the possibility that gamma-ray bursts (GRBs) are the sources of the ultra-high energy cosmic rays (UHECRs) within the internal shock model, assuming a pure proton composition of the UHECRs. For the first time, we combine the information from gamma-rays, cosmic rays, prompt neutrinos, and cosmogenic neutrinos quantitatively in a joint cosmic ray production and propagation model, and we show that the information on the cosmic energy budget can be obtained as a consequence. In addition to the neutron model, we consider alternative scenarios for the cosmic ray escape from the GRBs, i.e., that cosmic rays can leak from the sources. We find that the dip model, which describes the ankle in UHECR observations by the pair production dip, is strongly disfavored in combination with the internal shock model because a) unrealistically high baryonic loadings (energy in protons versus energy in electrons/gamma-rays) are needed for the individual GRBs and b) the prompt neutrino flux easily overshoots the corresponding neutrino bound. On the other hand, GRBs may account for the UHECRs in the ankle transition model if cosmic rays leak out from the source at the highest energies. In that case, we demonstrate that future neutrino observations can efficiently test most of the parameter space -- unless the baryonic loading is much larger than previously anticipated.

Philipp Baerwald; Mauricio Bustamante; Walter Winter

2014-01-08T23:59:59.000Z

419

Fermi LAT Observation of Diffuse Gamma-Rays Produced through Interactions Between Local Interstellar Matter and High Energy Cosmic Rays  

DOE Green Energy (OSTI)

Observations by the Large Area Telescope (LAT) on the Fermi mission of diffuse {gamma}-rays in a mid-latitude region in the third quadrant (Galactic longitude l from 200{sup o} to 260{sup o} and latitude |b| from 22{sup o} to 60{sup o}) are reported. The region contains no known large molecular cloud and most of the atomic hydrogen is within 1 kpc of the solar system. The contributions of {gamma}-ray point sources and inverse Compton scattering are estimated and subtracted. The residual {gamma}-ray intensity exhibits a linear correlation with the atomic gas column density in energy from 100 MeV to 10 GeV. The measured integrated {gamma}-ray emissivity is (1.63 {+-} 0.05) x 10{sup -26} photons s{sup -1}sr{sup -1} H-atom{sup -1} and (0.66 {+-} 0.02) x 10{sup -26} photons s{sup -1}sr{sup -1} H-atom{sup -1} above 100 MeV and above 300 MeV, respectively, with an additional systematic error of {approx}10%. The differential emissivity from 100 MeV to 10 GeV agrees with calculations based on cosmic ray spectra consistent with those directly measured, at the 10% level. The results obtained indicate that cosmic ray nuclei spectra within 1 kpc from the solar system in regions studied are close to the local interstellar spectra inferred from direct measurements at the Earth within {approx}10%.

Abdo, A.A.; /Naval Research Lab, Wash., D.C. /Federal City Coll.; Ackermann, M.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Ajello, M.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Atwood, W.B.; /UC, Santa Cruz; Axelsson, M.; /Stockholm U. /Stockholm U., OKC; Baldini, L.; /INFN, Pisa; Ballet, J.; /DAPNIA, Saclay; Barbiellini, G.; /INFN, Trieste /Trieste U.; Bastieri, D.; /INFN, Padua /Padua U.; Baughman, B.M.; /Ohio State U.; Bechtol, K.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bellazzini, R.; /INFN, Pisa; Berenji, B.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bloom, E.D.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bonamente, E.; /INFN, Perugia /Perugia U.; Borgland, A.W.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bregeon, J.; /INFN, Pisa; Brez, A.; /INFN, Pisa; Brigida, M.; /Bari U. /INFN, Bari; Bruel, P.; /Ecole Polytechnique; Burnett, T.H.; /Washington U., Seattle /Bari U. /INFN, Bari /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /IASF, Milan /Milan Polytechnic /Royal Inst. Tech., Stockholm /Stockholm U., OKC /DAPNIA, Saclay /INFN, Perugia /Perugia U. /NASA, Goddard /Naval Research Lab, Wash., D.C. /George Mason U. /NASA, Goddard /INFN, Perugia /Perugia U. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Montpellier U. /Stockholm U. /Stockholm U., OKC /Royal Inst. Tech., Stockholm /ASDC, Frascati /Naval Research Lab, Wash., D.C. /INFN, Trieste /Bari U. /INFN, Bari /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /CENBG, Gradignan /CENBG, Gradignan /Montpellier U. /Bari U. /INFN, Bari /Ecole Polytechnique /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /INFN, Trieste /Hiroshima U. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Bari U. /INFN, Bari /INFN, Bari; /more authors..

2012-03-30T23:59:59.000Z

420

Extracting cosmic microwave background polarisation from satellite astrophysical maps  

E-Print Network (OSTI)

We present the application of the Fast Independent Component Analysis technique for blind component separation to polarised astrophysical emission. We study how the Cosmic Microwave Background (CMB) polarised signal, consisting of $E$ and $B$ modes, can be extracted from maps affected by substantial contamination from diffuse Galactic foregrounds and instrumental noise. We perform the analysis of all sky maps simulated accordingly to the nominal performances of the Low Frequency Instrument (LFI) aboard the Planck satellite; the sky signal is modeled as a superposition of CMB, generated by a Gaussian, nearly scale invariant cosmological perturbation spectrum, and the existing simulated polarisation templates of Galactic synchrotron. Our results indicate that the angular power spectrum of CMB $E$ modes can be recovered on all scales up to $\\ell\\simeq 1000$, corresponding to the fourth acoustic oscillation, while $B$ modes can be detected, up to their turnover at $\\ell\\simeq 100$ if cosmological tensor amplitude...

Baccigalupi, C; De Zotti, G; Smoot, G F; Burigana, C; Maino, D; Bedini, L; Salerno, E

2002-01-01T23:59:59.000Z

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421

Non-Gaussianity and the Cosmic Microwave Background Anisotropies  

E-Print Network (OSTI)

We review in a pedagogical way the present status of the impact of non-Gaussianity (NG) on the Cosmic Microwave Background (CMB) anisotropies. We first show how to set the initial conditions at second-order for the (gauge invariant) CMB anisotropies when some primordial NG is present. However, there are many sources of NG in CMB anisotropies, beyond the primordial one, which can contaminate the primordial signal. We mainly focus on the NG generated from the post-inflationary evolution of the CMB anisotropies at second-order in perturbation theory at large and small angular scales, such as the ones generated at the recombination epoch. We show how to derive the equations to study the second-order CMB anisotropies and provide analytical computations to evaluate their contamination to primordial NG (complemented with numerical examples). We also offer a brief summary of other secondary effects. This review requires basic knowledge of the theory of cosmological perturbations at the linear level.

N. Bartolo; S. Matarrese; A. Riotto

2010-01-22T23:59:59.000Z

422

Amplified radio emission from cosmic ray air showers in thunderstorms  

E-Print Network (OSTI)

Cosmic ray air showers produce radio emission, consisting in large part of geosynchrotron emission. Since the radiation mechanism is based on particle acceleration, the atmospheric electric field can play an important role. Especially inside thunderclouds large electric fields can be present. We examine the contribution of an electric field to the emission mechanism theoretically and experimentally. Two mechanisms of amplification of radio emission are considered: the acceleration radiation of the shower particles and the radiation from the current that is produced by ionization electrons moving in the electric field. We selected and evaluated LOPES data recorded during thunderstorms, periods of heavy cloudiness and periods of cloudless weather. We find that during thunderstorms the radio emission can be strongly enhanced. No amplified pulses were found during periods of cloudless sky or heavy cloudiness, suggesting that the electric field effect for radio air shower measurements can be safely ignored during non-thunderstorm conditions.

Stijn Buitink; for the LOPES collaboration

2007-02-16T23:59:59.000Z

423

Superconducting cosmic strings as gamma ray burst engines  

E-Print Network (OSTI)

Cusps of superconducting strings can serve as GRB engines. A powerful beamed pulse of electromagnetic radiation from a cusp produces a jet of accelerated particles, whose propagation is terminated by the shock responsible for GRB. A single free parameter, the string scale of symmetry breaking $\\eta \\sim 10^{14} GeV$, together with reasonable assumptions about the magnitude of cosmic magnetic fields and the fraction of volume that they occupy, explains the GRB rate, duration and fluence, as well as the observed ranges of these quantities. The wiggles on the string can drive the short-time structures of GRB. This model predicts that GRBs are accompanied by strong bursts of gravitational radiation which should be detectable by LIGO, VIRGO and LISA detectors.

V. Berezinsky; B. Hnatyk; A. Vilenkin

2000-01-12T23:59:59.000Z

424

Cosmological and astrophysical constraints on superconducting cosmic strings  

E-Print Network (OSTI)

We investigate the cosmological and astrophysical constraints on superconducting cosmic strings (SCSs). SCS loops emit strong bursts of electromagnetic waves, which might affect various cosmological and astrophysical observations. We take into account the effect on the CMB anisotropy, CMB blackbody spectrum, BBN, observational implications on radio wave burst and X-ray or gamma-ray events, and stochastic gravitational wave background measured by pulsar timing experiments. We then derive constraints on the parameters of SCS from current observations and estimate prospects for detecting SCS signatures in on-going observations. As a result, we find that these constraints exclude broad parameter regions, and also that on-going radio wave observations can probe large parameter space.

Koichi Miyamoto; Kazunori Nakayama

2012-12-30T23:59:59.000Z

425

Price's law, mass inflation, and strong cosmic censorship  

E-Print Network (OSTI)

Two aspects of the widely accepted heuristic picture of the final state of gravitational collapse are the so-called Price law tails, describing the asymptotics of the exterior region of the black hole that forms, and Israel-Poisson's mass inflation scenario, describing the internal structure of the black hole. (The latter scenario, if valid, would indicate that the maximal development of initial data is extendible as a C^0 metric, putting into question the validity of Penrose's strong cosmic censorship conjecture.) In this talk, I shall discuss a series of rigorous results proving both Price's law and the mass inflation scenario in an appropriate spherically symmetric setting. The proof of Price's law is joint work with I. Rodnianski.

Mihalis Dafermos

2004-01-29T23:59:59.000Z

426

Dark Energy Constraints from the Cosmic Age and Supernova  

E-Print Network (OSTI)

Using the low limit of cosmic ages from globular cluster and the white dwarfs: $t_0 > 12$Gyr, together with recent new high redshift supernova observations from the HST/GOODS program and previous supernova data, we give a considerable estimation of the equation of state for dark energy, with uniform priors as weak as $0.2paper a new scenario of dark energy dubbed Quintom, which gives rise to the equation of state larger than -1 in the past and less than -1 today, satisfying current observations. In addition we've also considered the implications of recent X-ray gas mass fraction data on dark energy, which favors a negative running of the equation of state.

Bo Feng; Xiulian Wang; Xinmin Zhang

2004-04-11T23:59:59.000Z

427

Precision measurement of cosmic magnification from 21 cm emitting galaxies  

DOE Green Energy (OSTI)

We show how precision lensing measurements can be obtained through the lensing magnification effect in high redshift 21cm emission from galaxies. Normally, cosmic magnification measurements have been seriously complicated by galaxy clustering. With precise redshifts obtained from 21cm emission line wavelength, one can correlate galaxies at different source planes, or exclude close pairs to eliminate such contaminations. We provide forecasts for future surveys, specifically the SKA and CLAR. SKA can achieve percent precision on the dark matter power spectrum and the galaxy dark matter cross correlation power spectrum, while CLAR can measure an accurate cross correlation power spectrum. The neutral hydrogen fraction was most likely significantly higher at high redshifts, which improves the number of observed galaxies significantly, such that also CLAR can measure the dark matter lensing power spectrum. SKA can also allow precise measurement of lensing bispectrum.

Zhang, Pengjie; /Fermilab; Pen, Ue-Li; /Canadian Inst. Theor. Astrophys.

2005-04-01T23:59:59.000Z

428

Forecasting constraints on the cosmic duality relation with galaxy clusters  

E-Print Network (OSTI)

One of the fundamental hypotheses in observational cosmology is the validity of the so-called cosmic distance-duality relation (CDDR). In this paper, we perform Monte Carlo simulations based on the method developed in Holanda, Goncalves & Alcaniz (2012) [JCAP 1206 (2012) 022] to answer the following question: what is the number of galaxy clusters observations N_{crit} needed to check the validity of this relation at a given confidence level? At 2\\sigma, we find that N_{crit} should be increased at least by a factor of 5 relative to the current sample size if we assume the current observational uncertainty \\sigma_{obs}. Reducing this latter quantity by a factor of 2, we show that the present number of data would be already enough to check the validity of the CDDR at 2\\sigma.

R. S. Goncalves; J. S. Alcaniz; J. C. Carvalho; R. F. L. Holanda

2013-06-27T23:59:59.000Z

429

Cosmic Gamma-Ray Bursts The Remaining Mysteries  

E-Print Network (OSTI)

To anyone who has read a scientific journal or even a newspaper in the last six months, it might appear that cosmic gamma-ray bursts hold no more mysteries: they are cosmological, and possibly the most powerful explosions in the Universe. In fact, however, bursts remain mysterious in many ways. There is no general agreement upon the nature of the event which releases the initial energy. One burst at least appears to strain the energy budget of the merging neutron star model. There is evidence that another recent event may have come from a nearby supernova. Finally, while the number count statistics clearly show a strong deviation from the -3/2 power law expected for a Euclidean, homogeneous distribution, the distributions of some classes of bursts appear to follow a -3/2 power law rather closely. The recent data on bursts is reviewed, some of the mysteries discussed, and future experiments are outlined.

Hurley, K

1998-01-01T23:59:59.000Z

430

Commissioning of the ATLAS Muon Spectrometer with Cosmic Rays  

E-Print Network (OSTI)

The ATLAS detector at the Large Hadron Collider has collected several hundred million cosmic ray events during 2008 and 2009. These data were used to commission the Muon Spectrometer and to study the performance of the trigger and tracking chambers, their alignment, the detector control system, the data acquisition and the analysis programs. We present the performance in the relevant parameters that determine the quality of the muon measurement. We discuss the single element efficiency, resolution and noise rates, the calibration method of the detector response and of the alignment system, the track reconstruction efficiency and the momentum measurement. The results show that the detector is close to the design performance and that the Muon Spectrometer is ready to detect muons produced in high energy proton-proton collisions.

The ATLAS Collaboration

2010-06-22T23:59:59.000Z

431

Cosmic Ray Anomalies Inspired Some Discussion on Modified Chaplygin Gas  

E-Print Network (OSTI)

The postulation of Dark energy and Dark matter on the basis of observational results does not end the mystery of their existence. Theoretically new insights into dark matter have been achieved analyzing recent experimental data from the cosmic ray physics. It has been shown that, if the dark matter is a hidden scalar field, then it is not only possible to explain the ATIC/PPB BETS excess but also the observed dark matter abundance naturally and simultaneously. Being motivated, mainly by the assumption of hidden scalar field and some associated works, we consider the Modified Chaplygin Gas for some thermodynamical analysis. The point that if the scalar field is assumed to oscillate before the reheating was not completed, i.e., T_R importance of thermodynamical analysis. We, assuming the properties of Modified Chaplygin Gas, derive an expression for the second law of thermodynamics. It is obse...

Saikia, Julie

2009-01-01T23:59:59.000Z

432

Cosmic Ray Anomalies Inspired Some Discussion on Modified Chaplygin Gas  

E-Print Network (OSTI)

The postulation of Dark energy and Dark matter on the basis of observational results does not end the mystery of their existence. Theoretically new insights into dark matter have been achieved analyzing recent experimental data from the cosmic ray physics. It has been shown that, if the dark matter is a hidden scalar field, then it is not only possible to explain the ATIC/PPB BETS excess but also the observed dark matter abundance naturally and simultaneously. Being motivated, mainly by the assumption of hidden scalar field and some associated works, we consider the Modified Chaplygin Gas for some thermodynamical analysis. The point that if the scalar field is assumed to oscillate before the reheating was not completed, i.e., T_R importance of thermodynamical analysis. We, assuming the properties of Modified Chaplygin Gas, derive an expression for the second law of thermodynamics. It is observed that it also sheds some new lights on Generalised Second Law.

Julie Saikia; Balendra Kr. Dev Choudhury

2009-06-03T23:59:59.000Z

433

Ultra high energy cosmic rays and the large scale structure of the galactic magnetic field  

E-Print Network (OSTI)

We study the deflection of ultra high energy cosmic ray protons in different models of the regular galactic magnetic field. Such particles have gyroradii well in excess of 1 kpc and their propagation in the galaxy reflects only the large scale structure of the galactic magnetic field. A future large experimental statistics of cosmic rays of energy above 10$^{19}$ eV could be used for a study of the large scale structure of the galactic magnetic field if such cosmic rays are indeed charged nuclei accelerated at powerful astrophysical objects and if the distribution of their sources is not fully isotropic.

Todor Stanev

1996-07-17T23:59:59.000Z

434

Analytic Approaches to the Study of Small Scale Structure on Cosmic String Networks  

E-Print Network (OSTI)

We present an analytic model specifically designed to address the long standing issue of small scale structure on cosmic string networks. The model is derived from the microscopic string equations, together with a few motivated assumptions. The resulting form of the correlation between two points on a string is exploited to study smoothing by gravitational radiation, loop formation and lensing by cosmic strings. In addition, the properties of the small loop population and the possibility of detecting gravitational waves generated by their lowest harmonics are investigated. Whenever possible, we compare the predictions of the model to the most recent numerical simulations of cosmic string networks.

Jorge V. Rocha

2008-12-20T23:59:59.000Z

435

Cosmic ray physics in calculations of cosmological structure formation  

E-Print Network (OSTI)

Cosmic rays (CRs) play a decisive role within our own Galaxy. They provide partial pressure support against gravity, they trace past energetic events such as supernovae, and they reveal the underlying structure of the baryonic matter distribution through their interactions. To study the impact of CRs on galaxy and cosmic structure formation and evolution, we develop an approximative framework for treating dynamical and radiative effects of CRs in cosmological simulations. Our guiding principle is to try to find a balance between capturing as many physical properties of CR populations as possible while at the same time requiring as little extra computational resources as possible. We approximate the CR spectrum of each fluid element by a single power-law, with spatially and temporally varying normalisation, low-energy cut-off, and spectral index. Principles of conservation of particle number, energy, and pressure are then used to derive evolution equations for the basic variables describing the CR spectrum, both due to adiabatic and non-adiabatic processes. The processes considered include compression and rarefaction, CR injection via shocks in supernova remnants, injection in structure formation shock waves, in-situ re-acceleration of CRs, CR spatial diffusion, CR energy losses due to Coulomb interactions, ionisation losses, Bremsstrahlung losses, and, finally, hadronic interactions with the background gas, including the associated gamma-ray and radio emission due to subsequent pion decay. We show that the formalism reproduces CR energy densities, pressure, and cooling rates with an accuracy of ~10% in steady state conditions where CR injection balances cooling. Our framework is therefore well suited to be included into numerical simulation schemes of galaxy and structure formation. (abridged)

Torsten A. Ensslin; Christoph Pfrommer; Volker Springel; Martin Jubelgas

2006-03-17T23:59:59.000Z

436

30TH INTERNATIONAL COSMIC RAY CONFERENCE The VERITAS Trigger System  

E-Print Network (OSTI)

Abstract: The VERITAS gamma-ray observatory, situated in southern Arizona, is an array of four 12m diameter imaging Cherenkov telescopes, each with a 499-pixel photomultiplier-tube camera. The instrument is designed to detect astrophysical gamma rays at energies above 100 GeV. At the low end of the VERITAS energy range, fluctuations in the night sky background light and single muons from cosmic-ray showers constitute significant backgrounds. VERITAS employs a three-tier trigger system to reduce the rate of these background events: an initial trigger which acts at the single pixel level, a pattern trigger which acts on the relative timing and distribution of pixel-level triggers within a single telescope camera, and an array-level trigger which requires simultaneous observation of an air-shower event in multiple telescopes. This final coincidence requirement significantly reduces the rate of background events, particularly those due to single muons. In this paper, the implementation of all levels of the VERITAS trigger system is discussed and their joint performance is characterized. The VERITAS gamma-ray observatory, situated in southern Arizona, is an array of four 12m diameter imaging Cherenkov telescopes, each with a 499pixel photomultiplier-tube camera. The instrument is designed to detect astrophysical gamma rays with energies above 100 GeV. At the low end of the VERITAS energy range, fluctuations in the night sky background light (NSB) and single muons from cosmic-ray showers constitute significant backgrounds, which the three-tiered VERI-TAS trigger system is designed to reduce. VERITAS has operated in a three-telescope configuration with the full trigger system since December 2006. A fourth telescope was added to the array in

A. Weinstein; For The; Veritas Collaboration

2007-01-01T23:59:59.000Z

437

Determination of the Far-Infrared Cosmic Background Using COBE/DIRBE and WHAM Data  

E-Print Network (OSTI)

Determination of the cosmic infrared background (CIB) at far infrared wavelengths using COBE/DIRBE data is limited by the accuracy to which foreground interplanetary and Galactic dust emission can be modeled and subtracted. Previous determinations of the far infrared CIB (e.g., Hauser et al. 1998) were based on the detection of residual isotropic emission in skymaps from which the emission from interplanetary dust and the neutral interstellar medium were removed. In this paper we use the Wisconsin H-alpha Mapper (WHAM) Northern Sky Survey as a tracer of the ionized medium to examine the effect of this foreground component on determination of the CIB. We decompose the DIRBE far infrared data for five high Galactic latitude regions into H I and H-alpha correlated components and a residual component. We find the H-alpha correlated component to be consistent with zero for each region, and we find that addition of an H-alpha correlated component in modeling the foreground emission has negligible effect on derived CIB results. Our CIB detections and 2 sigma upper limits are essentially the same as those derived by Hauser et al. and are given by nu I_nu (nW m-2 sr-1) < 75, < 32, 25 +- 8, and 13 +- 3 at 60, 100, 140, and 240 microns, respectively. Our residuals have not been subjected to a detailed anisotropy test, so our CIB results do not supersede those of Hauser et al. We derive upper limits on the 100 micron emissivity of the ionized medium that are typically about 40% of the 100 micron emissivity of the neutral atomic medium. This low value may be caused in part by a lower dust-to-gas mass ratio in the ionized medium than in the neutral medium, and in part by a shortcoming of using H-alpha intensity as a tracer of far infrared emission.

N. Odegard; R. G. Arendt; E. Dwek; L. M. Haffner; M. G. Hauser; R. J. Reynolds

2007-05-27T23:59:59.000Z

438

Blazing Cerenkov Flashes at the Horizons by Cosmic Rays and Neutrinos Induced Air-Showers  

E-Print Network (OSTI)

High Energy Cosmic Rays (C.R.) versus Neutrino and Neutralino induced Air-Shower maybe tested at Horizons by their muons, gamma and Cerenkov blazing signals. Inclined and Horizontal C.R. Showers (70-90 zenith angle) produce secondary (gamma, e+, e-) mostly suppressed by high column atmosphere depth. Earliest shower Cherenkov photons are diluted by large distances and by air opacity, while secondary penetrating muons and their successive decay into electrons and gamma, may revive additional Cerenkov lights. GeVs gamma telescopes at the top of the mountains or in Space may detect at horizons PeVs up to EeV C.R. and their secondaries. Details on arrival angle and column depth, shower shape, timing signature of photon flash intensity, may inform us on the altitude interaction and primary UHECR composition. Below the horizons, at zenith angle among copious single albedo muons, rare up-going showers traced by muon bundles would give evidence of rare tau Earth-Skimming neutrinos, at EeVs energies. Their rate may be comparable with 6.3 PeVs anti-neutrino electron induced air-shower (mostly hadronic) originated above and also below horizons, in interposed atmosphere by W resonance at Glashow peak. Additional and complementary UHE SUSY neutralinos at tens PeVs-EeV energy may blaze, by its characteristic electromagnetic signature. Their secondary shower blazing Cerenkov lights and distances might be disentangled from UHECR by Stereoscopic Telescopes such as Magic ones or Hess array experiment. The horizontal detection sensitivity of Magic in the present set up (if totally devoted to the Horizons Shower search) maybe already be comparable to AMANDA underground neutrino detector at PeVs energies.

D. Fargion

2004-12-21T23:59:59.000Z

439

The relation between post-shock temperature, cosmic-ray pressure and cosmic-ray escape for non-relativistic shocks  

E-Print Network (OSTI)

Supernova remnants are thought to be the dominant source of Galactic cosmic rays. This requires that at least 5% of the available energy is transferred to cosmic rays, implying a high cosmic-ray pressure downstream of supernova remnant shocks. Recently, it has been shown that the downstream temperature in some remnants is low compared to the measured shock velocities, implying that additional pressure support by accelerated particles is present. Here we use a two-fluid thermodynamic approach to derive the relation between post-shock fractional cosmic-ray pressure and post-shock temperature, assuming no additional heating beyond adiabatic heating in the shock precursor and with all non-adiabatic heating occurring at the subshock. The derived relations show that a high fractional cosmic-ray pressure is only possible, if a substantial fraction of the incoming energy flux escapes from the system. Recently a shock velocity and a downstream proton temperature was measured for a shock in the supernova remnant RCW 86...

Vink, Jacco; Helder, E A; Schure, K M

2010-01-01T23:59:59.000Z

440

Attaining and using extremely high intensities of solar energy with non-imaging concentrators  

SciTech Connect

Using the principles and techniques of non-imaging optics, solar concentrations that approach the theoretical maximum can be achieved. In this paper, the authors review recent progress in attaining, measuring, and using such ultrahigh solar fluxes. In particular, they review the design principles for optimized two-stage concentrators and solar furnaces and discuss the characteristics and properties of a variety of non-imaging secondaries which have been employed. These include Compound Parabolic Concentrators (CPC) type secondaries, Dielectric Totally Internally Reflecting Concentrators (DTIRC), and flow-line or {open_quotes}trumpet{close_quotes} concentrators. The usual design is a configuration where {phi}, the rim angle of the primary, is small, that is, corresponding to a system with a relatively large focal length to diameter (F/D) ratio. All three types of secondary are characterized by a design acceptance angle {phi}{sub a} which must be greater than or equal to {phi}. The design parameters and trade-offs for each of these systems including strategies for choice of particular secondary and degree of truncation, are presented. The authors review the calorimetric techniques used to measure these high intensities and describe a newly developed technique for {open_quotes}extracting{close_quotes} light from inside a high index medium. Finally they review a number of potential applications for highly concentrated solar energy and the current status of the associated technology. By making possible new and unique applications for intense solar flux, these techniques have opened a whole new frontier for research and development of potential economic uses of solar energy. 63 refs., 34 figs., 3 tabs.

Jenkins, D.; O`Gallagher, J.; Winston, R.

1997-12-31T23:59:59.000Z

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441

Self-force on an electric dipole in the spacetime of a cosmic string  

E-Print Network (OSTI)

We calculate the electrostatic self-force on an electric dipole in the spacetime generated by a static, thin, infinite and straight cosmic string. The electric dipole is held fixed in different configurations, namely, parallel, perpendicular to the cosmic string and oriented along the azimuthal direction around this topological defect, which is stretched along the z axis. We show that the self-force is equivalent to an interaction of the electric dipole with an effective dipole moment which depends on the linear mass density of the cosmic string and on the configuration. The plots of the self-forces as functions of the parameter which determines the angular deficit of the cosmic string are shown for those different configurations.

C. R. Muniz; V. B Bezerra

2013-10-16T23:59:59.000Z

442

Neural networks and separation of cosmic microwave background and astrophysical signals in sky maps  

E-Print Network (OSTI)

Maps produced by large area surveys aimed at imaging primordial fluctuations of the Cosmic Microwave Background (CMB) contain a linear mixture of signals by several astrophysical and cosmological sources (Galactic synchrotron,

C. Baccigalupi; L. Bedini; C. Burigana; G. De Zotti; A. Farusi; D. Maino; M. Maris; F. Perrotta; E. Salerno; L. Toffolatti; A. Tonazzini

2000-01-01T23:59:59.000Z

443

PSU-PAL-99-1 Cosmic-Ray Positrons: Are There Primary Sources?  

E-Print Network (OSTI)

Galactic cosmic rays consist of primary and secondary particles. Primary cosmic rays are thought to be energized by first order Fermi acceleration processes at supernova shock fronts within our Galaxy. The cosmic rays that eventually reach the Earth from this source are mainly protons and atomic nuclei, but also include electrons. Secondary cosmic rays are created in collisions of primary particles with the diffuse interstellar gas. They are relatively rare but carry important information on the Galactic propagation of the primary particles. The secondary component includes a small fraction of antimatter particles, positrons and antiprotons. In addition, positrons and antiprotons may also come from unusual sources and possibly provide insight into new physics. For instance, the annihilation of heavy supersymmetric dark matter particles within the Galactic halo could lead to positrons or antiprotons with distinctive energy signatures. With the High-Energy

Stéphane Coutu; Steven W. Barwick; James J. Beatty; Amit Bhattacharyya; R. Bower; Christopher J. Chaput; Georgia A. De Nolfo; Michael A. Duvernois; Shawn P. Mckee; Dietrich Müller; James A. Musser; Scott L. Nutter; Simon P. Swordy; Gregory Tarlé; Andrew D. Tomasch; Eric Torbet

1999-01-01T23:59:59.000Z

444

Relative Composition and Energy Spectra of Light Nuclei in Cosmic Rays: Results from AMS-01  

E-Print Network (OSTI)

Measurement of the chemical and isotopic composition of cosmic rays is essential for the precise understanding of their propagation in the galaxy. While the model parameters are mainly determined using the B/C ratio, the ...

Becker, R.

445

Tanpopo cosmic dust collector: Silica aerogel production and bacterial DNA contamination analysis  

E-Print Network (OSTI)

Hydrophobic silica aerogels with ultra-low densities have been designed and developed as cosmic dust capture media for the Tanpopo mission which is proposed to be carried out on the International Space Station. Glass particles as a simulated cosmic dust with 30 \\mu m in diameter and 2.4 g/cm^3 in density were successfully captured by the novel aerogel at a velocity of 6 km/s. Background levels of contaminated DNA in the ultra-low density aerogel were lower than the detection limit of a polymerase chain reaction assay. These results show that the manufactured aerogel has good performance as a cosmic dust collector and sufficient quality in respect of DNA contamination. The aerogel is feasible for the biological analyses of captured cosmic dust particles in the astrobiological studies.

Tabata, Makoto; Yokobori, Shin-ichi; Kawai, Hideyuki; Takahashi, Jun-ichi; Yano, Hajime; Yamagishi, Akihiko

2011-01-01T23:59:59.000Z

446

First LIGO search for gravitational wave bursts from cosmic (super)strings  

E-Print Network (OSTI)

We report on a matched-filter search for gravitational wave bursts from cosmic string cusps using LIGO data from the fourth science run (S4) which took place in February and March 2005. No gravitational waves were detected ...

Zucker, Michael E.

447

Search for microquasar features in cosmic ray spectra with AMS-01  

E-Print Network (OSTI)

Accreting x-ray binaries are sometimes observed to emit compact, relativistic jets of cool plasma; these objects are called "microquasars". It is possible that these jets are responsible for a large flux of galactic cosmic ...

Monreal, Benjamin, 1977-

2004-01-01T23:59:59.000Z

448

Search for antideuterons and strangelets in cosmic rays with AMS-01  

E-Print Network (OSTI)

AMS (the Alpha Magnetic Spectrometer) is a high-energy particle detector in space. An engineer- ing version of AMS, AMS-01, flew on the space shuttle Discovery for ten days in June 1998 and collected 108 cosmic ray events. ...

Henning, Reyco, 1975-

2004-01-01T23:59:59.000Z

449

Solar Activity and Cloud Opacity Variations: A Modulated Cosmic Ray Ionization Model  

Science Conference Proceedings (OSTI)

The observed correlation between global low cloud amount and the flux of high energy cosmic rays supports the idea that ionization plays a crucial role in tropospheric cloud formation. This idea is explored quantitatively with a simple model ...

David Marsden; Richard E. Lingenfelter

2003-02-01T23:59:59.000Z

450

Gamma Ray Bursts Cannot Produce the Observed Cosmic Rays Above 10 19 eV  

E-Print Network (OSTI)

Received; accepted – 2 – Using recent results indicating that the redshift distribution of ?-ray bursts most likely follows the redshift evolution of the star formation rate, I show that the energy input from these bursts at low redshifts is insufficient to account for the observed flux of ultrahigh energy cosmic rays with energies above 1019 eV. Subject Headings: gamma-rays: bursts — cosmic rays: theory – 3 – 1.

F. W. Stecker

1999-01-01T23:59:59.000Z

451

The collision and snapping of cosmic strings generating spherical impulsive gravitational waves  

E-Print Network (OSTI)

The Penrose method for constructing spherical impulsive gravitational waves is investigated in detail, including alternative spatial sections and an arbitrary cosmological constant. The resulting waves include those that are generated by a snapping cosmic string. The method is used to construct an explicit exact solution of Einstein's equations describing the collision of two nonaligned cosmic strings in a Minkowski background which snap at their point of collision.

J. Podolsky; J. B. Griffiths

2000-01-17T23:59:59.000Z

452

Pierre Auger Enhancements: Transition from Galactic to Extragalactic Cosmic Ray Sources  

SciTech Connect

The Pierre Auger Collaboration has decided to include detector enhancements in order to have unitary detection efficiencies down to 1017 eV in cosmic rays detection. These enhancements consist in high elevation telescopes and an infill area with both surface detectors and underground muon counters thus allowing a detailed study of the spectrum region where the cosmic rays sources are assumed to change from galactic to extragalactic origins.

Etchegoyen, A. [Laboratorio Tandar - Comision Nacional de Energia Atomica, Buenos Aires (Argentina); Universidad Tecnologica Nacional, Regional Buenos Aires, Buenos Aires (Argentina); Melo, D.; Supanitsky, A. D. [Laboratorio Tandar - Comision Nacional de Energia Atomica, Buenos Aires (Argentina); Medina, M. C. [Laboratorio Tan