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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 Science Drivers of Particle Physics Energy Frontier Intensity Frontier Cosmic Frontier Theoretical Physics...

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

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

4

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

5

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

6

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

Office of Science (SC) Website

Energy Frontier High Energy Physics (HEP) HEP Home About Research Science Drivers of Particle Physics Energy Frontier Intensity Frontier Cosmic Frontier Theoretical Physics...

7

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

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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

9

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

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#SpaceWeek: Science on the Cosmic Frontier | Department of Energy  

Office of Environmental Management (EM)

SpaceWeek: Science on the Cosmic Frontier SpaceWeek: Science on the Cosmic Frontier March 3, 2014 - 12:00pm Addthis Join us for a Twitter

11

A STAGED MUON-BASED FACILITY TO ENABLE INTENSITY AND ENERGY FRONTIER SCIENCE IN THE US*  

E-Print Network (OSTI)

A STAGED MUON-BASED FACILITY TO ENABLE INTENSITY AND ENERGY FRONTIER SCIENCE IN THE US* Jean. It requires facilities at both high energy and high intensity frontiers. Neutrino oscillations are irrefutable precision flavour physics at the high intensity frontier. At the high energy frontier, a multi-TeV lepton

McDonald, Kirk

12

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

13

Working Group Report: Computing for the Intensity Frontier  

SciTech Connect

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.

Rebel, B.; Sanchez, M.C.; Wolbers, S.

2013-10-25T23:59:59.000Z

14

Issues and R&D Required for the Intensity Frontier Accelerators  

SciTech Connect

Operation, upgrade and development of accelerators for Intensity Frontier face formidable challenges in order to satisfy both the near-term and long-term Particle Physics program. Here we discuss key issues and R&D required for the Intensity Frontier accelerators.

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

2013-09-26T23:59:59.000Z

15

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

16

Planning the Future of U.S. Particle Physics (Snowmass 2013): Chapter 2: Intensity Frontier  

E-Print Network (OSTI)

These reports present the results of the 2013 Community Summer Study of the APS Division of Particles and Fields ("Snowmass 2013") on the future program of particle physics in the U.S. Chapter 2, on the Intensity Frontier, discusses the program of research with high-intensity beams and rare processes. This area includes experiments on neutrinos, proton decay, charged-lepton and quark weak interactions, atomic and nuclear probes of fundamental symmetries, and searches for new, light, weakly-interacting particles.

J. L. Hewett; H. Weerts; K. S. Babu; J. Butler; B. Casey; A. de Gouvea; R. Essig; Y. Grossman; D. Hitlin; J. Jaros; E. Kearns; K. Kumar; Z. Ligeti; Z. -T. Lu; K. Pitts; M. Ramsey-Musolf; J. Ritchie; K. Scholberg; W. Wester; G. P. Zeller

2014-01-23T23:59:59.000Z

17

Planning the Future of U.S. Particle Physics (Snowmass 2013): Chapter 2: Intensity Frontier  

E-Print Network (OSTI)

These reports present the results of the 2013 Community Summer Study of the APS Division of Particles and Fields ("Snowmass 2013") on the future program of particle physics in the U.S. Chapter 2, on the Intensity Frontier, discusses the program of research with high-intensity beams and rare processes. This area includes experiments on neutrinos, proton decay, charged-lepton and quark weak interactions, atomic and nuclear probes of fundamental symmetries, and searches for new, light, weakly-interacting particles.

Hewett, J L; Babu, K S; Butler, J; Casey, B; de Gouvea, A; Essig, R; Grossman, Y; Hitlin, D; Jaros, J; Kearns, E; Kumar, K; Ligeti, Z; Lu, Z -T; Pitts, K; Ramsey-Musolf, M; Ritchie, J; Scholberg, K; Wester, W; Zeller, G P

2014-01-01T23:59:59.000Z

18

Spatial Intensity Profiles of Galactic Cosmic Rays in the Heliosphere  

SciTech Connect

We study the spatial intensity profiles of galactic cosmic ray protons (H) and {alpha}-particles (He) during the solar minimum periods of 1987 (the so-called negative drift state) and 1977/1997 (both positive drift states) of the heliosphere. These intensities were measured with the Pioneer, Voyager and IMP spacecraft. The 1997 intensities were so low that one cannot readily explain them, even with the acceleration at the solar wind termination shock (SWTS) and modulation in the heliosheath included. Our heliospheric model is azimuthally symmetric with a spherical shock and heliopause, however, and we infer from its results that more realistic geometries may produce modulation effects that will explain the observations better.

Moraal, H. [School of Physics, Northwest University, Potchefstroom 2520 (South Africa); Caballero-Lopez, R.A.; McDonald, F.B. [Institute for Physical Science and Technology, University of Maryland, College Park, MD 20740 (United States)

2004-09-15T23:59:59.000Z

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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

20

Short-period variation of cosmic-ray intensity observed in the stratosphere  

Science Journals Connector (OSTI)

To investigate the variation of the cosmic-ray intensity in the Earth atmosphere, stratospheric balloon soundings are performed weekly at Campinas (Brazil...2 and 173 g/cm2. Apparently these oscillations are not ...

N. A. Van Bui; I. M. Martin; A. Turtelli jr.; Yu. I. Stozhkov

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

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

22

Differential directional intensities of low energy cosmic ray muons near sea level  

E-Print Network (OSTI)

DIFFERENTIAL DIRECTIOiNAL INTEiNSITIES OF LOW ENERGY COSMIC RAY MUONS liR SEA LEVEL A Thesis by DAVID RUDOLPH DURDA Submitted to the Graduate College of Texas ASM University in partial fulfillment of the requirement for the degree of MASTER... OF SCIENCE May 1970 Physics DIFFERENTIAL DIRECTIONAL INTENSITIES OF LOW ENERGY COSMIC RAY MUONS NEAR SEA LEVEL A Thesis by DAVID RUDOLPH DURDA Approved as to style and content by: C airman o Committee Hea o Department Me er Mem er May 1970...

Durda, David Rudolph

2012-06-07T23:59:59.000Z

23

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

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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

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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 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

27

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,

28

Solar, geomagnetic and cosmic ray intensity changes, preceding the cyclone appearances around Mexico  

Science Journals Connector (OSTI)

Recently it has been suggested that there exist specific changes in the cosmic ray intensity and some solar and geomagnetic parameters during the days, preceding the hurricane appearances over the North Atlantic Ocean. To understand better these phenomena, data for all hurricanes born not only over the Atlantic but also over the Pacific waters in the last 55 years that hit the Mexican borders were elaborated. As basic hurricane parameters the maximum rotational velocity and the estimated total energy were used. To avoid any interference all hurricanes, overlapping the preceding ones with more than 20 days were not included. Then the behavior of the cosmic ray (CR) intensity, the sunspot (SS) numbers, and the geomagnetic parameters (AP) and (KP) in 35 days prior and 20 days after the cyclone start were investigated. The CR, SS, AP and KP showed much more intensive disturbances in the periods preceding and following the hurricane appearance. For SS this disturbance gradually increase with the hurricane strength. A characteristic peak in the CR intensity appears before the hurricane start. But its place varies between 5 and 20 days before that start. Specific changes were observed in the SS. For major hurricanes they begins sometimes more than 20 days in advance. The AP and the KP show series of bursts, spread over the whole period of 30 preceding days. The obtained results from the performed correlational analysis are enough interesting to motivate a further statistical analysis with more precise techniques: in particular a common periodicity of 30 years found in the number of tropical storms landing into Mexico, the averaged rotational wind velocity and the ACE must be studied in connection with the solar Hale cycle. Using coherence wavelet spectral analysis we present a comparative study between one terrestrial and one cosmophysical phenomena that presumable influence hurricanes development: African dust outbreaks versus cosmic rays for all North Atlantic tropical cyclones. It is shown that the cosmophysical influence cannot be considered as a negligible effect.

J. Prez-Peraza; S. Kavlakov; V. Velasco; A. Gallegos-Cruz; E. Azpra-Romero; O. Delgado-Delgado; F. Villicaa-Cruz

2008-01-01T23:59:59.000Z

29

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

30

24. Cosmic rays 1 24. COSMIC RAYS  

E-Print Network (OSTI)

electrons, protons and helium, as well as carbon, oxygen, iron, and other nuclei synthesized in stars) and the intensity of the cosmic rays with energies below about 10 GeV. In addition, the lower-energy cosmic rays the intensity of any component of the cosmic radiation in the GeV range depends both on the location and time

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26. Cosmic rays 1 26. COSMIC RAYS  

E-Print Network (OSTI)

electrons, protons and helium, as well as carbon, oxygen, iron, and other nuclei synthesized in stars) and the intensity of the cosmic rays with energies below about 10 GeV. In addition, the lower-energy cosmic rays the intensity of any component of the cosmic radiation in the GeV range depends both on the location and time

32

Fermilab Facts:  

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

program pushes forward on three interrelated frontiers of particle physics: the Energy Frontier, the Intensity Frontier and the Cosmic Frontier. * Fermilab experiments at...

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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 Science Drivers of Particle Physics Energy Frontier Intensity Frontier Cosmic Frontier...

34

Frontiers in Science Lectures  

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

or Neither? The new science of epigenetics Exploring Mars: Curiosity and its laser Higgs Boson and Beyond: The quest for new laws of physics Frontiers in Science Lectures...

35

Telecommunications Frontier Client Installation  

E-Print Network (OSTI)

Telecommunications Frontier Client Installation 1. Fax the completed form to 979.847.1111. 2 Signature Date Telecommunications Office Use Only Service Due Date: Installation Cost: Billed To: Print Form

36

Environmental Frontier of Sustainability  

E-Print Network (OSTI)

A A Global Environmental Studies Frontier of Sustainability Science Akihisa MORI, Global Environmental Studies Satoshi KONISHI, Institute of Advanced Energy, etc Integrated Research Bld, economics, energy, architecture, meteorology and biology and so on. In this sense, this class welcomes

Takada, Shoji

37

Muon Colliders: The Next Frontier  

SciTech Connect

Muon Colliders provide a path to the energy frontier in particle physics but have been regarded to be "at least 20 years away" for 20 years. I will review recent progress in design studies and hardware R&D and show that a Muon Collider can be established as a real option for the post-LHC era if the current vigorous R&D effort revitalized by the Muon Collider Task Force at Fermilab can be supported to its conclusion. All critical technologies are being addressed and no show-stoppers have emerged. Detector backgrounds have been studied in detail and appear to be manageable and the physics can be done with existing detector technology. A muon facility can be built through a staged scenario starting from a low-energy muon source with unprecedented intensity for exquisite reach for rare processes, followed by a Neutrino Factory with ultrapure neutrino beams with unparalleled sensitivity for disentangling neutrino mixing, leading to an energy frontier Muon Collider with excellent energy resolution.

Yagmur Tourun

2009-07-29T23:59:59.000Z

38

Muon Colliders: The Next Frontier  

ScienceCinema (OSTI)

Muon Colliders provide a path to the energy frontier in particle physics but have been regarded to be "at least 20 years away" for 20 years. I will review recent progress in design studies and hardware R&D and show that a Muon Collider can be established as a real option for the post-LHC era if the current vigorous R&D effort revitalized by the Muon Collider Task Force at Fermilab can be supported to its conclusion. All critical technologies are being addressed and no show-stoppers have emerged. Detector backgrounds have been studied in detail and appear to be manageable and the physics can be done with existing detector technology. A muon facility can be built through a staged scenario starting from a low-energy muon source with unprecedented intensity for exquisite reach for rare processes, followed by a Neutrino Factory with ultrapure neutrino beams with unparalleled sensitivity for disentangling neutrino mixing, leading to an energy frontier Muon Collider with excellent energy resolution.

Yagmur Tourun

2010-01-08T23:59:59.000Z

39

Intensity of the Soft and Hard Component of the Cosmic Radiation as a Function of Altitude at Geomagnetic Latitudes of 28N, 41N, and 55N  

Science Journals Connector (OSTI)

Counter telescopes have been flown with plastic balloons to a maximum altitude of 94,000 ft. Intensity vs pressure curves have been obtained at geomagnetic latitudes of ?=55?,41?,and28? for the total cosmic radiation and for the components capable of traversing several thickness of lead. The energy spectrum of primary cosmic-ray particles has been derived from the extrapolation of the intensity of the total radiation to the top of the atmosphere. The integral momentum spectrum of the total primary radiation is given by N(>pcZe)=0.49(pcZe)-1.0. The results show that the radiation originating from primaries in the energy range 1 to 4 Bev (cut-off energies at ?=55?and41?) is predominantly of a nucleonic nature. The absence of an appreciable electronic component can be explained by assuming that, close to the top of the atmosphere, electrons originate predominantly from the decay of neutral mesons and that, within this energy range, the over-all probability of nucleon emission is greater than that of meson production. In sharp contrast, the soft component originating from primaries in the range from 4 to 8 Bev (cut-off at ?=41?and28?) multiplies rapidly in the atmosphere. This large transition effect in air with a maximum at about 10 cm Hg pressure is very characteristic of electron showers. It is concluded that the probability of neutral mesons being produced is comparatively high at primary energies between 4 and 8 Bev. At energies higher than 8 Bev this effect is even more pronounced, due to the contribution of the plural and multiple production of mesons.

Marcello L. Vidale

1952-10-15T23:59:59.000Z

40

Theoretical Physics | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

High Energy Physics (HEP) HEP Home About Research Science Drivers of Particle Physics Energy Frontier Intensity Frontier Cosmic Frontier Theoretical Physics Unique Aspects and...

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.


41

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

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

Accelerator & Detector Physics Computing CMS Detector Intensity Frontier Cosmic Frontier Works in Progress Energy Frontier Large Hadron Collider The LHC at CERN, the European...

42

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

Office of Science (SC) Website

High Energy Physics (HEP) HEP Home About Research Science Drivers of Particle Physics Energy Frontier Intensity Frontier Cosmic Frontier Theoretical Physics Advanced Technology...

43

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

Office of Science (SC) Website

Research High Energy Physics (HEP) HEP Home About Research Science Drivers of Particle Physics Energy Frontier Intensity Frontier Cosmic Frontier Theoretical Physics Advanced...

44

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

E-Print Network (OSTI)

that energy intensity is not necessarily a good indicator of energy efficiency, whereas by controllingUS 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

45

2014 Frontier Fiesta University of Houston  

E-Print Network (OSTI)

2014 Frontier Fiesta University of Houston Building Codes & Regulations #12;#12;University of Houston Frontier Fiesta Association FrontierFiesta2014 www.uh.edu/fiesta | March 20-22, 2014 | 3 TABLE Frontier Fiesta Association Director of Operations ffops@central.uh.edu #12;FrontierFiesta2014 University

Azevedo, Ricardo

46

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

47

Frontiers In Quantitative  

E-Print Network (OSTI)

-in-Publication Data: ISBN-13: 978-0-470-29292-1 Printed in the United States of America 10 9 8 7 6 5 4 3 2 1 iv #12;P1 the United States at (317) 572-3993 or fax (317) 572-4002. Wiley also publishes its books in a varietyFrontiers In Quantitative FinanceVolatility and Credit Risk Modeling RAMA CONT #12;P1: a/b P2: c

Cont, Rama

48

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)

49

1CHILE'S FRONTIER FORESTS: CONSERVING A GLOBAL TREASURE FRONTIER FORESTS  

E-Print Network (OSTI)

A GLOBAL TREASURE Eduardo Neira HernánVerscheure CarmenRevenga Map production and GIS Analysis Eduardo. BIBLIOGRAPHY 39 ANNEX I: MAPS OF FRONTIER FORESTS, OTHER VEGETATIVE COVER, PROTECTED AREAS, AND FOREST: CONSERVING A GLOBAL TREASURE LIST OF MAPS Map 1 Frontier forests, other vegetative cover, protected areas

50

1CHILE'S FRONTIER FORESTS: CONSERVING A GLOBAL TREASURE FRONTIER FORESTS  

E-Print Network (OSTI)

A GLOBAL TREASURE Eduardo Neira HernánVerscheure CarmenRevenga Map production and GIS Analysis Eduardo 4.4.4 Altered or disturbed forests 35 5. CONCLUSIONS 37 6. BIBLIOGRAPHY 39 ANNEX I: MAPS OF FRONTIER OF MAPS Map 1 Frontier forests, other vegetative cover, protected areas, and forest activities

51

Bake Fiesta 2014 Frontier Fiesta  

E-Print Network (OSTI)

CookOff & Bake Fiesta forms 2014 #12;2014 Frontier Fiesta Cook-Off Registration Form To register and reserve your site for the Cook-Off, please complete the following information and submit all for 2014 Frontier Fiesta Cook-Off: Beans Brisket Ribs Chicken Fajita Our team needs: _______ site fee

Azevedo, Ricardo

52

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...

53

Environmental Frontier of Sustainability Science  

E-Print Network (OSTI)

A Global Environmental Studies Frontier of Sustainability Science Akihisa MORI, Global Environmental Studies Satoshi KONISHI, Institute of Advanced Energy, etc Master July 14, politics, economics, energy, architecture, meteorology and marine science and so on. In this sense

Takada, Shoji

54

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":""}]}

55

Photo of the Week: The Cosmic Frontier | Department of Energy  

Office of Environmental Management (EM)

which is a research collaboration between institutions from the U.S., Brazil, U.K., Germany, Spain and Switzerland. The survey aims to explore the dynamics of the...

56

Neutron stars is focus of Los Alamos National Laboratory Frontiers...  

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

Frontiers in Science lectures Neutron stars is focus of Los Alamos National Laboratory Frontiers in Science lectures Lectures are intended to increase local public awareness of the...

57

Apply: Building Energy Efficiency Frontiers and Incubator Technologies...  

Energy Savers (EERE)

Apply: Building Energy Efficiency Frontiers and Incubator Technologies (BENEFIT) - 2014 (DE-FOA-0001027) Apply: Building Energy Efficiency Frontiers and Incubator Technologies...

58

Frontiers, Opportunities, and Challenges in Biochemical and Chemical...  

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

Frontiers, Opportunities, and Challenges in Biochemical and Chemical Catalysis of CO2. Frontiers, Opportunities, and Challenges in Biochemical and Chemical Catalysis of CO2....

59

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

Office of Science (SC) Website

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...

60

Energy Frontier Research in Extreme Environments (EFree) | U...  

Office of Science (SC) Website

Frontier Research in Extreme Environments (EFree) Energy Frontier Research Centers (EFRCs) EFRCs Home Centers EFRC External Websites Research Science Highlights News & Events...

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

Department of Energy Hosts Inaugural Energy Frontier Research...  

Office of Science (SC) Website

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

62

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

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

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...

63

Cosmic Structures  

Science Journals Connector (OSTI)

In this first chapter, the cosmic players (objects) are introduced superficially, whose detailed properties will then entertain us to the end of the book. The play starts in front of our doors, with the Solar Sys...

Professor Dr. Wolfgang Kundt

2001-01-01T23:59:59.000Z

64

Frontiers in Biological Sciences Seminar Series Presents  

E-Print Network (OSTI)

Frontiers in Biological Sciences Seminar Series Presents Integrated Molecular Approaches to Study Professor, Departments of Earth and Planetary Science and Environmental Science, Policy, Management) methods with geochemical approaches, it has been possible to begin to determine how these communities

65

Nucleon measurements at the precision frontier  

SciTech Connect

We comment on nucleon measurements at the precision frontier. As examples of what can be learned, we concentrate on three topics, which are parity violating scattering experiments, the proton radius puzzle, and the symbiosis between nuclear and atomic physics.

Carlson, Carl E. [Physics Department, College of William and Mary, Williamsburg, VA 23187 (United States)

2013-11-07T23:59:59.000Z

66

Hayden White: Frontiers of Consciousness at UCSC  

E-Print Network (OSTI)

of consciousness. Hayden White: Frontiers of Consciousnessyou had a very motley crew. White: A motley crew, to put itIn the capitalist context. White: You can sell the human,

UCSC Library, Regional History Project; White, Hayden; Vanderscoff, Cameron

2013-01-01T23:59:59.000Z

67

Microfluidics Expanding the Frontiers of Microbial Ecology  

E-Print Network (OSTI)

Microfluidics has significantly contributed to the expansion of the frontiers of microbial ecology over the past decade by allowing researchers to observe the behaviors of microbes in highly controlled microenvironments, ...

Rusconi, Roberto

68

Cosmic Rays and Global Warming  

E-Print Network (OSTI)

It has been claimed by others that observed temporal correlations of terrestrial cloud cover with `the cosmic ray intensity' are causal. The possibility arises, therefore, of a connection between cosmic rays and Global Warming. If true, the implications would be very great. We have examined this claim to look for evidence to corroborate it. So far we have not found any and so our tentative conclusions are to doubt it. Such correlations as appear are more likely to be due to the small variations in solar irradiance, which, of course, correlate with cosmic rays. We estimate that less than 15% of the 11-year cycle warming variations are due to cosmic rays and less than 2% of the warming over the last 35 years is due to this cause.

T. Sloan; A W Wolfendale

2007-06-28T23:59:59.000Z

69

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/

70

Forests and climate change focus of Frontiers in Science lectures  

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

Frontiers in Science lectures Forests and climate change focus of Frontiers in Science lectures LANL researcher Nate McDowell will discuss climate change and its effects on forest...

71

Cosmical Electrodynamics  

Science Journals Connector (OSTI)

A review is given of the development in the field of cosmical electrodynamics. It is mentioned that the great interest in thermonuclear research has produced a considerable progress in plasma physics. This is of astrophysical interest because it is now possible to check the theories of a plasma by experiment.

H. Alfvn

1960-01-01T23:59:59.000Z

72

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":""}]}

73

AMERICAN FRONTIERS: CRITICAL HISTORIES WINTER 2006 SYLLABUS  

E-Print Network (OSTI)

since the late 19th century; the social transformation of the American West in the 20th century; and images of the frontier and the West in American culture since the early 20th century. We will also Publisher: W. W. Norton; Reprint edition (January 30, 1987) Roaring Camp: The Social World of the California

74

Research frontiers in the physical sciences  

Science Journals Connector (OSTI)

...publication receipt of abstracts by Editor 30 October...overview of current research To get some feel for...water, waves, wave energy d (v) waterway engineering...water, waves, wave energy) d (v) Phil. Trans...Lond. A (2002) Research frontiers in the physical...

2002-01-01T23:59:59.000Z

75

Nanometric Optical Imaging Frontiers in Chemical Imaging  

E-Print Network (OSTI)

Nanometric Optical Imaging Frontiers in Chemical Imaging Seminar Series Presented by... Professor growing field which has provided for nanometric optical imaging in the near-field. Even though a variety of techniques are being developed with nanometric optical imaging potential, near-field optics remains the most

76

Frontiers of biomedical text mining: current progress  

E-Print Network (OSTI)

Frontiers of biomedical text mining: current progress Pierre Zweigenbaum, Dina Demner-Fushman, Hong of biomedical text mining continue to present interesting challenges and opportunities for great improvements and interesting research. In this article we review the current state of the art in biomedical text mining or `Bio

Yu, Hong

77

Cosmic Glows  

E-Print Network (OSTI)

This is the obligatory Cosmic Microwave Background review. I discuss the current status of CMB anisotropies, together with some points on the related topic of the Far-Infrared Background. We have already learned a number of important things from CMB anisotropies. Models which are in good shape have: approximately flat geometry; cold dark-matter, plus something like a cosmological constant; roughly scale invariant adiabatic fluctuations; and close to Gaussian statistics. The constraints from the CMB are beginning to be comparable to those from other cosmological measurements. With a wealth of new data coming in, it is expected that CMB anisotropies will soon provide the most stringent limits on fundamental cosmological parameters, as well as probing high energy particle physics and the Dark Ages of astrophysics. Nudge, nudge. Wink, wink. Say no more.

Douglas Scott

1999-12-02T23:59:59.000Z

78

Frontiers in Planetary and Stellar Magnetism through High-Performance...  

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

Hwang, project co-PI Frontiers in Planetary and Stellar Magnetism through High-Performance Computing PI Name: Jonathan Aurnou PI Email: aurnou@ucla.edu Institution: University...

79

Earthquake triggering discussed in three Frontiers in Science...  

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

causes is the topic of the next series of Frontiers in Science lectures by Paul Johnson. November 6, 2014 Paul Johnson Paul Johnson Contact Steve Sandoval Communications...

80

Light-Material Interactions in Energy Conversion - Energy Frontier...  

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

The recorded presentations and panel discussion are now available for online viewing. The Light-Material Interactions in Energy Conversion Energy Frontier Research Center...

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

Frontiers in Energy Research: Soaking Up the Sunshine | Photosynthetic...  

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

Sunshine July 13, 2012 Frontiers in Energy Research: Soaking Up the Sunshine Biohybrid light antennas offer more efficient solar energy capture than natural systems Read PARC...

82

Light-Material Interactions in Energy Conversion - Energy Frontier...  

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

Si as part of RG-3 research efforts (Chris Gladden, LBNL) The Scientific Vision of the "Light-Material Interactions in Energy Conversion Energy Frontier Research Center"...

83

Light-Material Interactions in Energy Conversion - Energy Frontier...  

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

Millikan Board Room map California Institute of Technology Pasadena, CA The Light-Material Interactions in Energy Conversion (LMI) Energy Frontier Research Center...

84

Light-Material Interactions in Energy Conversion - Energy Frontier...  

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

of Energy Steven Chu visits Caltech labs For more information or questions about the Light-Material Interactions in Energy Conversion Energy Frontier Research Center, please...

85

Light-Material Interactions in Energy Conversion - Energy Frontier...  

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

event details 02.06.13 logo Redefining the Limits of Photovoltaic Efficiency The LMI Energy Frontier Research Center, along with the Resnick Sustainability Institute, is...

86

Data Intensive  

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

Data Intensive Data Intensive Computing Pilot Program In 2014 NERSC is conducting its second and last round of allocations to projects in data intensive science. This pilot aims to...

87

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...

88

SciTech Connect: Energy Frontier Research Center Center for Materials...  

Office of Scientific and Technical Information (OSTI)

Technical Report: Energy Frontier Research Center Center for Materials Science of Nuclear Fuels Citation Details In-Document Search Title: Energy Frontier Research Center Center...

89

PNNLs Data Intensive Computing research battles Homeland Security threats  

ScienceCinema (OSTI)

The Pacific Northwest National Laboratorys (PNNL's) approach to data intensive computing (DIC) is focused on three key research areas: hybrid hardware architecture, software architectures, and analytic algorithms. Advancements in these areas will help to address, and solve, DIC issues associated with capturing, managing, analyzing and understanding, in near real time, data at volumes and rates that push the frontiers of current technologies.

David Thurman; Joe Kielman; Katherine Wolf; David Atkinson

2012-12-31T23:59:59.000Z

90

PNNL pushing scientific discovery through data intensive computing breakthroughs  

ScienceCinema (OSTI)

The Pacific Northwest National Laboratorys approach to data intensive computing (DIC) is focused on three key research areas: hybrid hardware architectures, software architectures, and analytic algorithms. Advancements in these areas will help to address, and solve, DIC issues associated with capturing, managing, analyzing and understanding, in near real time, data at volumes and rates that push the frontiers of current technologies.

Deborah Gracio; David Koppenaal; Ruby Leung

2012-12-31T23:59:59.000Z

91

PNNLs Data Intensive Computing research battles Homeland Security threats  

SciTech Connect

The Pacific Northwest National Laboratorys (PNNL's) approach to data intensive computing (DIC) is focused on three key research areas: hybrid hardware architecture, software architectures, and analytic algorithms. Advancements in these areas will help to address, and solve, DIC issues associated with capturing, managing, analyzing and understanding, in near real time, data at volumes and rates that push the frontiers of current technologies.

David Thurman; Joe Kielman; Katherine Wolf; David Atkinson

2009-12-01T23:59:59.000Z

92

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.

93

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

94

Dark Matter Theory  

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

Dark Matter Theory Dark Matter Theory Understanding discoveries at the Energy, Intensity, and Cosmic Frontiers Get Expertise Rajan Gupta (505) 667-7664 Email Bruce Carlsten (505)...

95

Quantum Field Theory & Gravity  

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

Field Theory & Gravity Quantum Field Theory & Gravity Understanding discoveries at the Energy, Intensity, and Cosmic Frontiers Get Expertise Rajan Gupta (505) 667-7664 Email...

96

Particle Astrophysics  

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

Particle Astrophysics Particle Astrophysics Understanding discoveries at the Energy, Intensity, and Cosmic Frontiers Get Expertise Rajan Gupta (505) 667-7664 Email Bruce Carlsten...

97

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"

98

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."

99

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.

100

The proton engineering frontier project: Applications of accelerator technology  

Science Journals Connector (OSTI)

Launched in 2002 as a major national R&D project of Korea, the Proton Engineering Frontier Project is now being successfully completed ... of accelerator technologies. Developments of low energy ion accelerators,...

Kui Young Kim; Jae Sang Lee; Jae-Won Park

2012-07-01T23:59:59.000Z

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.


101

Light-Material Interactions in Energy Conversion - Energy Frontier...  

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

which authors are part of the LMI-EFRC: "A.A.A. was supported as part of the DOE "Light-Material Interactions in Energy Conversion' Energy Frontier Research Center under...

102

EFRC Overview | University of Texas Energy Frontier Research...  

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

About the EFRC The Center for Nano- and Molecular Science and Technology (CNM) at The University of Texas at Austin is the site of an Energy Frontier Research Center (EFRC) funded...

103

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.

104

Light-Material Interactions in Energy Conversion - Energy Frontier...  

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

Light Matters Video The LMI-EFRC Video "Light Matters" was the winner of the "Life at the Frontiers of Energy Research" video contest for striking photography and visual impact....

105

Two-Stroke Engines: New Frontier in Engine Efficiency  

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

Companies are revisiting two-stroke engines in the hopes of finding a new frontier in engine efficiency without the additional cost. But, not all two-stroke engines are the same.

106

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)  

SciTech Connect

'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) [Director, Center for Solar and Thermal Energy Conversion, University of Michigan; CSTEC Staff

2011-05-01T23:59:59.000Z

107

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)  

ScienceCinema (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

2011-11-02T23:59:59.000Z

108

Fort Inge and the Texas frontier, 1849-1869  

E-Print Network (OSTI)

the Civil War. Personalities associated with the history of Fort Inge include frontier artist Captain Seth Eastman, Frederick Law Olmsted, Bigfoot Wallace, Lydia Spencer Lane, and army officers such as William J. Hardee, Edmund Kirby Smith, Eugene A. Carr..., Gordon Granger, Zenas R. Bliss, William "Wild Bill" Hazen, John L. Bullis, and Fitzhugh Lee. This case study examines a number of topical problems associated with the U. S. Army and the frontier. Was the Army s role as an economic multiplier and mar...

Smith, Thomas Tyree

2012-06-07T23:59:59.000Z

109

Cosmic Ray Astronomy  

E-Print Network (OSTI)

Cosmic ray astronomy attempts to identify and study the sources of ultrahigh energy cosmic rays. It is unique in its reliance on charged particles as the information carriers. While no discrete source of ultrahigh energy cosmic rays has been identified so far, a new generation of detectors is acquiring the huge exposure that is needed at the highest energies, where deflection by magnetic fields is minimized and the background from distant sources is eliminated by pion photoproduction. In this paper, we summarize the status of cosmic ray astronomy, describing the detectors and the analysis techniques.

Paul Sommers; Stefan Westerhoff

2008-02-09T23:59:59.000Z

110

Origin of Cosmic Radiation  

E-Print Network (OSTI)

I give a brief overview of cosmic ray physics, highlighting some key questions and how they will be addressed by new experiments.

Thomas K. Gaisser

2000-11-28T23:59:59.000Z

111

Cosmic Radiation and Cancer  

Science Journals Connector (OSTI)

...methylcholanthrene in sesame oil and distributed...thickness for the production of small cosmic...optimum for the production of larger cosmic...results from the production of showers or...result of the cumulative and additive...atomic energy field and the consequent...Evanston, Illinois Botanical Sciences...

Frank H. J. Figge

1947-03-28T23:59:59.000Z

112

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

113

Polarization Observations with the Cosmic Background Imager  

E-Print Network (OSTI)

Polarization observations of the cosmic microwave background with the Cosmic Background Imager from September 2002 to May 2004 provide a significant detection of the E-mode polarization and reveal an angular power spectrum of polarized emission showing peaks and valleys that are shifted in phase by half a cycle relative to those of the total intensity spectrum. This key agreement between the phase of the observed polarization spectrum and that predicted based on the total intensity spectrum provides support for the standard model of cosmology, in which dark matter and dark energy are the dominant constituents, the geometry is close to flat, and primordial density fluctuations are predominantly adiabatic with a matter power spectrum commensurate with inflationary cosmological models.

A. C. S. Readhead; S. T. Myers; T. J. Pearson; J. L. Sievers; B. S. Mason; C. R. Contaldi; J. R. Bond; R. Bustos; P. Altamirano; C. Achermann; L. Bronfman; J. E. Carlstrom; J. K. Cartwright; S. Casassus; C. Dickinson; W. L. Holzapfel; J. M. Kovac; E. M. Leitch; J. May; S. Padin; D. Pogosyan; M. Pospieszalski; C. Pryke; R. Reeves; M. C. Shepherd; S. Torres

2004-09-23T23:59:59.000Z

114

Characterization and fluid flow simulation of naturally fractured Frontier sandstone, Green River Basin, Wyoming  

SciTech Connect

Significant gas reserves are present in low-permeability sandstones of the Frontier Formation in the greater Green River Basin, Wyoming. Successful exploitation of these reservoirs requires an understanding of the characteristics and fluid-flow response of the regional natural fracture system that controls reservoir productivity. Fracture characteristics were obtained from outcrop studies of Frontier sandstones at locations in the basin. The fracture data were combined with matrix permeability data to compute an anisotropic horizontal permeability tensor (magnitude and direction) corresponding to an equivalent reservoir system in the subsurface using a computational model developed by Oda (1985). This analysis shows that the maximum and minimum horizontal permeability and flow capacity are controlled by fracture intensity and decrease with increasing bed thickness. However, storage capacity is controlled by matrix porosity and increases linearly with increasing bed thickness. The relationship between bed thickness and the calculated fluid-flow properties was used in a reservoir simulation study of vertical, hydraulically-fractured and horizontal wells and horizontal wells of different lengths in analogous naturally fractured gas reservoirs. The simulation results show that flow capacity dominates early time production, while storage capacity dominates pressure support over time for vertical wells. For horizontal wells drilled perpendicular to the maximum permeability direction a high target production rate can be maintained over a longer time and have higher cumulative production than vertical wells. Longer horizontal wells are required for the same cumulative production with decreasing bed thickness.

Harstad, H. [New Mexico Tech, Socorro, NM (United States); Teufel, L.W.; Lorenz, J.C.; Brown, S.R. [Sandia National Labs., Albuquerque, NM (United States). Geomechanics Dept.

1996-08-01T23:59:59.000Z

115

A tale of two roads: Land tenure, poverty, and politics on the Guatemalan frontier  

E-Print Network (OSTI)

Salvador, Brazil. 742 Bunker, S.G. , 1984. Underdevelopingfrontiers in (e.g. , 314 Bunker, 1984), frontier settlers in

Carr, D

2006-01-01T23:59:59.000Z

116

Supplementary material to "Curvature and frontier orbital energies in density functional theory", by Stein et al.  

E-Print Network (OSTI)

Supplementary material to "Curvature and frontier orbital energies in density functional theory and frontier orbital energies in density functional theory", by Stein et al. 2. Calculation of curvature from: [{ }] [{ }] #12;Supplementary material to "Curvature and frontier orbital energies in density functional theory

Baer, Roi

117

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

118

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

119

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

120

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

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

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

122

Magnetic Monopoles and Cosmic Inflation  

E-Print Network (OSTI)

It is possible that the expansion of the universe began with an inflationary phase, in which the inflaton driving the process also was a Higgs field capable of stabilizing magnetic monopoles in a grand-unified gauge theory. If so, then the smallness of intensity fluctuations observed in the cosmic microwave background radiation implies that the self-coupling of the inflaton-Higgs field was exceedingly weak. It is argued here that the resulting broad, flat maximum in the Higgs potential makes the presence or absence of a topological zero in the field insignificant for inflation. There may be monopoles present in the universe, but the universe itself is not in the inflating core of a giant magnetic monopole.

Alfred Scharff Goldhaber

2005-12-09T23:59:59.000Z

123

Cosmic rays in astrospheres  

E-Print Network (OSTI)

Cosmic rays passing through large astrospheres can be efficiently cooled inside these "cavities" in the interstellar medium. Moreover, the energy spectra of these energetic particles are already modulated in front of the astrospherical bow shocks. We study the cosmic ray flux in and around lambda Cephei as an example for an astrosphere. The large-scale plasma flow is modeled hydrodynamically with radiative cooling. We studied the cosmic ray flux in a stellar wind cavity using a transport model based on stochastic differential equations. The required parameters, most importantly, the elements of the diffusion tensor, are based on the heliospheric parameters. The magnetic field required for the diffusion coefficients is calculated kinematically. We discuss the transport in an astrospheric scenario with varying parameters for the transport coefficients. We show that large stellar wind cavities can act as sinks for the galactic cosmic ray flux and thus can give rise to small-scale anisotropies in the direction to...

Scherer, Klaus; Bomans, Dominik; Ferreira, Stefan; Fichtner, Horst; Kleimann, Jens; Strauss, Dutoit; Weis, Kerstin; Wiengarten, Tobias; Wodzinski, Thomas

2015-01-01T23:59:59.000Z

124

Cosmic Abundance of Boron  

Science Journals Connector (OSTI)

... of low energy cosmic rays might be the necessary mechanism to produce the additional boron.Boron-10 is produced by the reaction 13C(p,a)10B, which has a Q value ...

A. G. W. CAMERON; S. A. COLGATE; L. GROSSMAN

1973-05-25T23:59:59.000Z

125

Cosmic Ray Physics  

E-Print Network (OSTI)

Cosmic ray story begins at the beginning of XX century. More then 100 years later, most of the main issues are still open questions, as sources, acceleration mechanism, propagation and composition. There is a continuing fascination with the studies of cosmic radiation mostly from the several contradictions connected to its observation. The radiation has an energy spectrum ranging from $\\sim$ 1 GeV to beyond 10$^{20}$ eV with a flux going from 1 particle per m$^2$ per $\\mu$s to less then 1 particle per km$^2$ per century, and so very different experimental techniques are needed to perform cosmic ray measurements in the different energy intervals. In this contribution the actual experimental status of cosmic ray knowledge will be reviewed.

D'Urso, Domenico

2014-01-01T23:59:59.000Z

126

Mechanized Silica Nanoparticles: A New Frontier in Theranostic Nanomedicine  

Science Journals Connector (OSTI)

Mechanized Silica Nanoparticles: A New Frontier in Theranostic Nanomedicine ... This article is part of the Theranostic Nanomedicine special issue. ... With the growth of nanomedicine, one can envisage the possibility of fabricating a theranostic vector that could release powerful therapeutics and diagnostic markers simultaneously and selectively to diseased tissue. ...

Michael W. Ambrogio; Courtney R. Thomas; Yan-Li Zhao; Jeffrey I. Zink; J. Fraser Stoddart

2011-06-15T23:59:59.000Z

127

Invited Paper New Frontiers of Network Security: The Threat Within  

E-Print Network (OSTI)

Invited Paper New Frontiers of Network Security: The Threat Within Sugata Sanyal1 , Ajit Shelat2% of information security threats originate from inside the organization. The instances of insider threats have. The Insider threats are generally caused by current or ex-employees, contractors or partners, who have

Sanyal, Sugata

128

Phenomenological Quantum Gravity: the birth of a new frontier?  

E-Print Network (OSTI)

In the last years a general consensus has emerged that, contrary to intuition, quantum-gravity effects may have relevant consequences for the propagation and interaction of high energy particles. This has given birth to the field of ``Phenomenological Quantum Gravity'' We review some of the aspects of this new, very exciting frontier of Physics.

R. Aloisio; P. Blasi; A. Galante; P. L. Ghia; A. F. Grillo; F. Mendez

2005-02-01T23:59:59.000Z

129

New Frontiers in Solar Physics: Broadband Imaging Spectroscopy with the  

E-Print Network (OSTI)

, the solar panel of the AASC recommended an integrated suite of instrumentation designed to meetNew Frontiers in Solar Physics: Broadband Imaging Spectroscopy with the Frequency Agile Solar and other astrophysical objects and processes. Outstanding problems in solar physics include the magnetic

130

Self-excited cosmic string dynamos  

Science Journals Connector (OSTI)

... When an oscillating cosmic ... cosmic string loop crosses a stationary magnetic field line, two sets of charge carriers are produced. ...

David N. Spergel; William H. Press; Robert J. Scherrer

1988-08-25T23:59:59.000Z

131

Cosmic ray research Public lecture  

E-Print Network (OSTI)

energy cosmic rays in Argentina 2 p.m., Wednesday, October 6, 2010 128 Jabara Hall Watkins Visiting powerful, high-energy cosmic rays that periodically bombard Earth. The project includes more than 450

132

DARK MATTER Tracing the "Cosmic Web" with Diffuse Gas  

E-Print Network (OSTI)

1 DARK MATTER STARS GAS NEUTRAL HYDROGEN Tracing the "Cosmic Web" with Diffuse Gas Quasar Quasar Absorption Lines Keck/HIRES Quasar Spectrum Observer baryons dark matter potential isotropic UV only on and the radiation field intensity... H I #12;5 GOAL: the primordial dark matter power spectrum

Steidel, Chuck

133

September 2, 2014 HighPower Targetry in Support of the Intensity Frontier  

E-Print Network (OSTI)

materials and in particular on the lowering of material fracture toughness. The resistance to thermal, coefficient of thermal expansion, and Young's modulus. Knowledge of these parameters for materials which load in the target, and iii) an understanding of the physical limits of the target material

McDonald, Kirk

134

2011 Intensity -1 INTENSITY OF SOUND  

E-Print Network (OSTI)

the rate at which energy is passing a certain point. This concept involves sound intensity. Consider the sound intensity. Recall the time rate of energy transfer is called "power". Thus, sound intensity2011 Intensity - 1 INTENSITY OF SOUND The objectives of this experiment are: · To understand

Glashausser, Charles

135

Further Study of Cosmic Rays on the Pacific Ocean  

Science Journals Connector (OSTI)

Records of cosmic-ray intensity obtained on the R. M. S. Aorangi during 15 new voyages between Vancouver, Canada, and Sydney, Australia, from July 28, 1937, to September 23, 1938, with a Carnegie model C cosmic-ray meter, are discussed and compared with records taken during 11 voyages on the same route previously reported by Compton and Turner. The observed minimum of cosmic-ray intensity near the equator averages 10.3 percent less than the intensity at Vancouver, in good agreement with the value given by Compton and Turner. The correlation between the cosmic-ray intensity and the atmospheric temperature is confirmed. An atmospheric temperature coefficient is found to be a function of latitude, with its highest numerical value of -0.25 percent per C for latitudes higher than 40 (N and S). With this variable temperature coefficient a latitude effect (about 8.5 percent) of magnetic origin alone is found. The mean latitude effect curve for 25 trips, corrected for external temperature, is flat beyond the critical latitudes (about 40N and 38S). The difference in cosmic-ray intensity between the Northern and Southern Hemispheres beyond the critical latitudes after this temperature correction is found to be 00.1 percent (probable error). This is inconsistent with a galactic rotation effect as great as the 0.5 percent predicted by Compton and Getting, but does not definitely rule out a more recent modification of their calculation. The origin of the latitude effect knee is ascribed to the minimum energy required for a primary electron to produce mesotrons capable of traversing the atmosphere. The small magnitude of the latitude effect is shown to supply strong evidence of the secondary nature of mesotrons.

Piara S. Gill

1939-06-15T23:59:59.000Z

136

Perimeter Institute Cosmic Acceleration  

E-Print Network (OSTI)

Wayne Hu Perimeter Institute April 2010 Cosmic Acceleration Dark Energy v. Modified Gravity #12;Outline · Dark Energy vs Modified Gravity · Three Regimes of Modified Gravity · Worked (Toy) Models: f 1998 Discovery #12;Mercury or Pluto? General relativity says Gravity = Geometry And Geometry = Matter-Energy

Hu, Wayne

137

Cosmic strings and superstrings  

Science Journals Connector (OSTI)

...different from unity, the standard field-theory value, then...mu and P, hence to rule out standard field-theory cosmic strings...interest, and allow us to plan further observations to probe...Anniversary Series: a collection of reviews celebrating the Royal Societys...

2010-01-01T23:59:59.000Z

138

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":""}]}

139

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.

140

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;

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.


141

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

142

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

143

Count data stochastic frontier models, with an application to the patentsR&D relationship  

Science Journals Connector (OSTI)

This article introduces a new count data stochastic frontier model that researchers can use ... patents awarded to a firm given expenditure on R&D.

Eduardo F; Richard Hofler

2013-06-01T23:59:59.000Z

144

Informational Webinar: Frontier Observatory for Research in Geothermal Energy (FORGE) Funding Opportunity Announcement  

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

The Energy Department will present a live webinar titled Frontier Observatory for Research in Geothermal Energy (FORGE) Funding Opportunity Announcement Informational Webinar," focusing on the...

145

Cosmic Rays on the Pacific Ocean  

Science Journals Connector (OSTI)

Records of cosmic-ray intensity obtained on the R. M. S. Aorangi during 12 voyages between Vancouver, Canada and Sydney, Australia, from March 17, 1936, to January 18, 1937, using a Carnegie model C cosmic-ray meter, are described and discussed. Typical records exhibiting the latitude effect are shown. A summary of the data taken at sea is given in the form of graphs, in which each datum point represents the average of 6 hours readings with a probable statistical error of 0.13 percent. Any variations due to a possible temperature coefficient of the instrument are negligible. The observed minimum of cosmic-ray intensity near the equator averages 10.3 percent less than the intensity at Vancouver, in satisfactory agreement, considering the difference in expermental conditions, with earlier measurements. The critical latitudes above which changes in intensity are less rapid, are found to be somewhat lower, 38.4N and 34.2S, than previously reported, and beyond these latitudes the intensity is found to continue to increase with latitude. At the higher latitudes is observed a variation, which appears to be seasonal, with the maximum in the cold months in both hemispheres. This variation is closely correlated with the atmospheric temperature. It is hence ascribed to changes in some atmospheric barrier of unknown nature, such as perhaps an atmospheric potential gradient, of whose strength the temperature of the atmosphere is an approximate but not exact index. Changes in this atmospheric barrier have been approximately allowed for by determining the external temperature coefficient and correcting the observations accordingly (this external temperature coefficient is comparable with that reported by Hess and his collaborators). The latitude effect curves as thus corrected should show the effect of the earth's magnetic field alone. They are now nearly flat beyond the critical latitudes and show a magnetic latitude effect of about 7.2 percent. This implies that a latitude effect of about 3.1 percent owes its origin to the atmospheric barrier. Seasonal variations in the corrected latitude effect curve are almost eliminated. Geomagnetic analysis of the energy distribution of the rays indicates a prominent component with a sharp energy threshold of about 7.5109 ev, and a component so weak as to be questionable, whose energy threshold is not greater than 2.5109 ev. It is not found possible to explain the 7.5109 ev threshold in terms of atmospheric absorption as has previously been supposed. Two alternative interpretations are suggested. The difference in cosmic-ray intensity between the northern and southern hemispheres under comparable conditions, as calculated from these data in various ways, appears to be no larger than the probable error of about 0.1 percent. This result is in conflict with the prediction by Compton and Getting of an excess in the north of about 0.5 percent, due to the motion of the earth with the rotation of the galaxy, but is not inconsistent with the small diurnal variation that has been found to follow sidereal time, if it is supposed that the cosmic rays acquire a part of the galactic motion.

A. H. Compton and R. N. Turner

1937-10-15T23:59:59.000Z

146

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.

147

Understanding the cosmic web  

E-Print Network (OSTI)

We investigate the characteristics and the time evolution of the cosmic web from redshift, z=2, to present time, within the framework of the NEXUS+ algorithm. This necessitates the introduction of new analysis tools optimally suited to describe the very intricate and hierarchical pattern that is the cosmic web. In particular, we characterize filaments (walls) in terms of their linear (surface) mass density. This is very good in capturing the evolution of these structures. At early times the cosmos is dominated by tenuous filaments and sheets, which, during subsequent evolution, merge together, such that the present day web is dominated by fewer, but much more massive, structures. We also show that voids are more naturally described in terms of their boundaries and not their centres. We illustrate this for void density profiles, which, when expressed as a function of the distance from void boundary, show a universal profile in good qualitative agreement with the theoretical shell-crossing framework of expandin...

Cautun, Marius; Jones, Bernard J T; Frenk, Carlos S

2015-01-01T23:59:59.000Z

148

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)  

ScienceCinema (OSTI)

'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

2011-11-03T23:59:59.000Z

149

Estimation and decomposition of cost efficiency in the health care food service sector: an extended stochastic frontier approach  

Science Journals Connector (OSTI)

......frontier approach|health...Journal of Management Mathematics...frontier approach A. ASSAF School of Management, University...Technology and Management. London...Ap- plied Science. MCPROUD...analysis approaches. Fish......

A. Assaf; K. M. Matawie

2008-01-01T23:59:59.000Z

150

Cosmic superstrings and primordial magnetogenesis  

Science Journals Connector (OSTI)

Cosmic superstrings are produced at the end of brane inflation. Their properties are similar to cosmic strings arising in grand unified theories. Like cosmic strings they can give rise to a primordial magnetic field, as a result of vortical motions stirred in the ionized plasma by the gravitational pull of moving string segments. The resulting magnetic field is both strong enough and coherent enough to seed the galactic dynamo and explain the observed magnetic fields of the galaxies.

Anne-Christine Davis and Konstantinos Dimopoulos

2005-08-19T23:59:59.000Z

151

The Origin of Cosmic Rays  

ScienceCinema (OSTI)

Cosmic Rays reach the Earth from space with energies of up to more than 1020 eV, carrying information on the most powerful particle accelerators that Nature has been able to assemble. Understanding where and how cosmic rays originate has required almost one century of investigations, and, although the last word is not written yet, recent observations and theory seem now to fit together to provide us with a global picture of the origin of cosmic rays of unprecedented clarity. Here we will describe what we learned from recent observations of astrophysical sources (such as supernova remnants and active galaxies) and we will illustrate what these observations tell us about the physics of particle acceleration and transport. We will also discuss the ?end? of the Galactic cosmic ray spectrum, which bridges out attention towards the so called ultra high energy cosmic rays (UHECRs). At ~1020 eV the gyration scale of cosmic rays in cosmic magnetic fields becomes large enough to allow us to point back to their sources, thereby allowing us to perform ?cosmic ray astronomy?, as confirmed by the recent results obtained with the Pierre Auger Observatory. We will discuss the implications of these observations for the understanding of UHECRs, as well as some questions which will likely remain unanswered and will be the target of the next generation of cosmic ray experiments.

Pasquale Blasi

2010-01-08T23:59:59.000Z

152

Intense Muon Beams for Experiments at Project X  

SciTech Connect

A coherent approach for providing muon beams to several experiments for the intensity-frontier program at Project X is described. Concepts developed for the front end of a muon collider/neutrino factory facility, such as phase rotation and ionization cooling, are applied, but with significant differences. High-intensity experiments typically require high-duty-factor beams pulsed at a time interval commensurate with the muon lifetime. It is challenging to provide large RF voltages at high duty factor, especially in the presence of intense radiation and strong magnetic fields, which may preclude the use of superconducting RF cavities. As an alternative, cavities made of materials such as ultra-pure Al and Be, which become very good but not super conductors at cryogenic temperatures, can be used.

C.M. Ankenbrandt, R.P. Johnson, C. Y. Yoshikawa, V.S. Kashikhin, D.V. Neuffer, J. Miller, R.A. Rimmer

2011-03-01T23:59:59.000Z

153

The efficient frontier for a portfolio that includes one risk-free asset  

Science Journals Connector (OSTI)

This paper presents a description of the efficient frontier of a portfolio composed by three assets, including a risk-free asset. We use a data analysis method to obtain two classes of assets and then we estimate the risk of each asset corresponding ... Keywords: efficient frontier, optimization, portfolio selection, principal component analysis, risk estimation

Florentin Serban; Maria Viorica Stefanescu; Silvia Dedu

2011-07-01T23:59:59.000Z

154

Research on Offshore Foundations: Papers at the International Symposium on Frontiers in  

E-Print Network (OSTI)

Research on Offshore Foundations: Papers at the International Symposium on Frontiers in Offshore@eng.ox.ac.uk http://www-civil.eng.ox.ac.uk/ #12;Research on Offshore Foundations: Papers at the International Symposium on Frontiers in Offshore Geotechnics Perth, Australia, 2005 G.T. Houlsby, C.M. Martin, B.W. Byrne

Byrne, Byron

155

FRONTIER, MAGNETIC, ELLIPSOMETRIC AND TIME-RESOLVED INFRARED SPECTROSCOPY (FIS + MET)  

E-Print Network (OSTI)

FRONTIER, MAGNETIC, ELLIPSOMETRIC AND TIME-RESOLVED INFRARED SPECTROSCOPY (FIS + MET) SCIENTIFIC-resolved Frontier Infrared Spectroscopy (FIS) and Magnetic, Ellipsometric and Time-Resolved Infrared Spectroscopy Beamline Team STAFF Larry Carr: MET lead beamline scientist Zhenxian Liu (CIW): FIS lead beamline scientist

Ohta, Shigemi

156

Power System Extreme Event Detection: The Vulnerability Frontier Bernard C. Lesieutre Ali Pinar  

E-Print Network (OSTI)

Power System Extreme Event Detection: The Vulnerability Frontier Bernard C. Lesieutre Ali Pinar the number of line outages in a grid to the power disrupted by the outages. This frontier describes the boundary of a space relating the possible severity of a disturbance in terms of power disruption, from zero

Pinar, Ali

157

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

158

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.

159

Expanding the Frontiers of Visual Analytics and Visualization  

SciTech Connect

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 Jims 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

160

The Very Large Hadron Collider: The farthest energy frontier  

SciTech Connect

The Very Large Hadron Collider (or Eloisatron) represents what may well be the final step on the energy frontier of accelerator-based high energy physics. While an extremely high luminosity proton collider at 100-200 TeV center of mass energy can probably be built in one step with LHC technology, that machine would cost more than what is presently politically acceptable. This talk summarizes the strategies of collider design including staged deployment, comparison with electron-positron colliders, opportunities for major innovation, and the technical challenges of reducing costs to manageable proportions. It also presents the priorities for relevant R and D for the next few years.

Barletta, William A.

2001-06-21T23:59:59.000Z

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

Simulating Cosmic Reionization  

E-Print Network (OSTI)

The Cosmic Dark Ages and the Epoch of Reionization constitute a crucial missing link in our understanding of the evolution of the intergalactic medium and the formation and evolution of galaxies. Due to the complex nature of this global process it is best studied through large-scale numerical simulations. This presents considerable computational challenges. The dominant contributors of ionizing radiation were dwarf galaxies. These tiny galaxies must be resolved in very large cosmological volumes in order to derive their clustering properties and the corresponding observational signatures correctly, which makes this one of the most challenging problems of numerical cosmology. We have recently performed the largest and most detailed simulations of the formation of early cosmological large-scale structures and their radiative feedback leading to cosmic reionization. This was achieved by running extremely large (up to 29 billion-particle) N-body simulations of the formation of the Cosmic Web, with enough particles and sufficient force resolution to resolve all the galactic halos with total masses larger than 10^8 Solar masses in computational volumes of up to (163 Mpc)^3. These results were then post-processed by propagating the ionizing radiation from all sources by using fast and accurate ray-tracing radiative transfer method. Both of our codes are parallelized using a combination of MPI and OpenMP and to this date have been run efficiently on up to 2048 cores (N-body) and up to 10000 cores (radiative transfer) on the newly-deployed Sun Constellation Linux Cluster at the Texas Advanced Computing Center. In this paper we describe our codes, parallelization strategies, scaling and some preliminary scientific results. (abridged)

Ilian T. Iliev; Paul R. Shapiro; Garrelt Mellema; Hugh Merz; Ue-Li Pen

2008-06-17T23:59:59.000Z

162

The Cosmic Horizon  

E-Print Network (OSTI)

The cosmological principle, promoting the view that the universe is homogeneous and isotropic, is embodied within the mathematical structure of the Robertson-Walker (RW) metric. The equations derived from an application of this metric to the Einstein Field Equations describe the expansion of the universe in terms of comoving coordinates, from which physical distances may be derived using a time-dependent expansion factor. These coordinates, however, do not explicitly reveal properties of the cosmic spacetime manifested in Birkhoff's theorem and its corollary. In this paper, we compare two forms of the metric--written in (the traditional) comoving coordinates, and a set of observer-dependent coordinates--first for the well-known de Sitter universe containing only dark energy, and then for a newly derived form of the RW metric, for a universe with dark energy and matter. We show that Rindler's event horizon--evident in the co-moving system--coincides with what one might call the "curvature horizon" appearing in the observer-dependent frame. The advantage of this dual prescription of the cosmic spacetime is that with the latest WMAP results, we now have a much better determination of the universe's mass-energy content, which permits us to calculate this curvature with unprecedented accuracy. We use it here to demonstrate that our observations have probed the limit beyond which the cosmic curvature prevents any signal from having ever reached us. In the case of de Sitter, where the mass-energy density is a constant, this limit is fixed for all time. For a universe with a changing density, this horizon expands until de Sitter is reached asymptotically, and then it too ceases to change.

Fulvio Melia

2007-11-27T23:59:59.000Z

163

Cosmic-ray Muon Radiography of a Volcano Seismo Seminor at Caltech, Nov 5, 2004  

E-Print Network (OSTI)

of the high-energy cosmic-ray muons passing through a mountain. This technique is in principle, based upon) with a mean energy of a few GeV (109 eV). Such high-energy muons have been used to explore the internal. It is also known that horizontally arriving cosmic-ray muons have a strong intensity in the high energy

Heaton, Thomas H.

164

Cosmic Rays and Experiment CZELTA  

SciTech Connect

This paper gives a review of the physics of cosmic rays with emphasis on the methods of detection and study. A summary is given of the Czech project CZELTA which is part of a multinational program to study cosmic rays with energies above 10{sup 14} eV.

Smolek, Karel; Nyklicek, Michal [Institute of Experimental and Applied Physics, Czech Technical University in Prague, Horska 3a/22, 128 00 Prague 2 (Czech Republic); Kovacikova, Petra [Faculty of Philosophy and Science, Silesian University in Opava, Bezrucovo namesti 13, 746 01 Opava (Czech Republic)

2007-11-26T23:59:59.000Z

165

The Cosmic Background Imager  

E-Print Network (OSTI)

The Cosmic Background Imager (CBI) is an instrument designed to make images of the cosmic microwave background radiation and to measure its statistical properties on angular scales from about 3 arc minutes to one degree (spherical harmonic scales from l ~ 4250 down to l ~ 400). The CBI is a 13-element interferometer mounted on a 6 meter platform operating in ten 1-GHz frequency bands from 26 GHz to 36 GHz. The instantaneous field of view of the instrument is 45 arcmin (FWHM) and its resolution ranges from 3 to 10 arcmin; larger fields can be imaged by mosaicing. At this frequency and resolution, the primary foreground is due to discrete extragalactic sources, which are monitored at the Owens Valley Radio Observatory and subtracted from the CBI visibility measurements. The instrument has been making observations since late 1999 of both primordial CMB fluctuations and the Sunyaev-Zeldovich effect in clusters of galaxies from its site at an altitude of 5080 meters near San Pedro de Atacama, in northern Chile. Observations will continue until August 2001 or later. We present preliminary results from the first few months of observations.

T. J. Pearson; B. S. Mason; S. Padin; A. C. S. Readhead; M. C. Shepherd; J. Sievers; P. S. Udomprasert; J. K. Cartwright

2000-12-11T23:59:59.000Z

166

The Cosmic Background Imager  

E-Print Network (OSTI)

Design and performance details are given for the Cosmic Background Imager (CBI), an interferometer array that is measuring the power spectrum of fluctuations in the cosmic microwave background radiation (CMBR) for multipoles in the range 400 < l < 3500. The CBI is located at an altitude of 5000 m in the Atacama Desert in northern Chile. It is a planar synthesis array with 13 0.9-m diameter antennas on a 6-m diameter tracking platform. Each antenna has a cooled, low-noise receiver operating in the 26-36 GHz band. Signals are cross-correlated in an analog filterbank correlator with ten 1 GHz bands. This allows spectral index measurements which can be used to distinguish CMBR signals from diffuse galactic foregrounds. A 1.2 kHz 180-deg phase switching scheme is used to reject cross-talk and low-frequency pick-up in the signal processing system. The CBI has a 3-axis mount which allows the tracking platform to be rotated about the optical axis, providing improved (u,v) coverage and a powerful discriminant against false signals generated in the receiving electronics. Rotating the tracking platform also permits polarization measurements when some of the antennas are configured for the orthogonal polarization.

S. Padin; M. C. Shepherd; J. K. Cartwright; R. G. Keeney; B. S. Mason; T. J. Pearson; A. C. S. Readhead; W. L. Schaal; J. Sievers; P. S. Udomprasert; J. K. Yamasaki; W. L. Holzapfel; J. E. Carlstrom; M. Joy; S. T. Myers; A. Otarola

2001-10-05T23:59:59.000Z

167

Vibration intensity difference thresholds.  

E-Print Network (OSTI)

??The intensity difference threshold is defined as the difference in the intensity of two stimuli which is just sufficient for their difference to be detected. (more)

Forta, Nazim Gizem

2009-01-01T23:59:59.000Z

168

Cosmic strings from preheating  

Science Journals Connector (OSTI)

We investigate nonthermal phase transitions that may occur after post-inflationary preheating in a simple model of a two-component scalar field with the effective potential ?(?i2?v2)2/4, where ?1 is identified with the inflaton field. We use three-dimensional lattice simulations to investigate the full nonlinear dynamics of the model. Fluctuations of the fields generated during and after preheating temporarily make the effective potential convex in the ?1 direction. The subsequent nonthermal phase transition with symmetry breaking leads to formation of cosmic strings even for v?1016 GeV. This mechanism of string formation, in a modulated (by the oscillating field ?1) phase transition, is different from the usual Kibble mechanism.

I. Tkachev; S. Khlebnikov; L. Kofman; A. Linde

1998-01-01T23:59:59.000Z

169

THE COSMIC ORIGINS SPECTROGRAPH  

SciTech Connect

The Cosmic Origins Spectrograph (COS) is a moderate-resolution spectrograph with unprecedented sensitivity that was installed into the Hubble Space Telescope (HST) in 2009 May, during HST Servicing Mission 4 (STS-125). We present the design philosophy and summarize the key characteristics of the instrument that will be of interest to potential observers. For faint targets, with flux F{sub {lambda}} Almost-Equal-To 1.0 Multiplication-Sign 10{sup -14} erg cm{sup -2} s{sup -1} A{sup -1}, COS can achieve comparable signal to noise (when compared to Space Telescope Imaging Spectrograph echelle modes) in 1%-2% of the observing time. This has led to a significant increase in the total data volume and data quality available to the community. For example, in the first 20 months of science operation (2009 September-2011 June) the cumulative redshift pathlength of extragalactic sight lines sampled by COS is nine times than sampled at moderate resolution in 19 previous years of Hubble observations. COS programs have observed 214 distinct lines of sight suitable for study of the intergalactic medium as of 2011 June. COS has measured, for the first time with high reliability, broad Ly{alpha} absorbers and Ne VIII in the intergalactic medium, and observed the He II reionization epoch along multiple sightlines. COS has detected the first CO emission and absorption in the UV spectra of low-mass circumstellar disks at the epoch of giant planet formation, and detected multiple ionization states of metals in extra-solar planetary atmospheres. In the coming years, COS will continue its census of intergalactic gas, probe galactic and cosmic structure, and explore physics in our solar system and Galaxy.

Green, James C.; Michael Shull, J.; Snow, Theodore P.; Stocke, John [Department of Astrophysical and Planetary Sciences, University of Colorado, 391-UCB, Boulder, CO 80309 (United States); Froning, Cynthia S.; Osterman, Steve; Beland, Stephane; Burgh, Eric B.; Danforth, Charles; France, Kevin [Center for Astrophysics and Space Astronomy, University of Colorado, 389-UCB, Boulder, CO 80309 (United States); Ebbets, Dennis [Ball Aerospace and Technologies Corp., 1600 Commerce Street, Boulder, CO 80301 (United States); Heap, Sara H. [NASA Goddard Space Flight Center, Code 681, Greenbelt, MD 20771 (United States); Leitherer, Claus; Sembach, Kenneth [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Linsky, Jeffrey L. [JILA, University of Colorado and NIST, Boulder, CO 80309-0440 (United States); Savage, Blair D. [Department of Astronomy, University of Wisconsin-Madison, 475 North Charter Street, Madison, WI 53706 (United States); Siegmund, Oswald H. W. [Astronomy Department, University of California, Berkeley, CA 94720 (United States); Spencer, John; Alan Stern, S. [Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302 (United States); Welsh, Barry [Space Sciences Laboratory, University of California, 7 Gauss Way, Berkeley, CA 94720 (United States); and others

2012-01-01T23:59:59.000Z

170

Physics Advisory Committee Meeting November 3-5, 2008  

E-Print Network (OSTI)

in the Particle Physics Project Prioritization Panel (P5) report to HEPAP--the Energy Frontier, the Intensity matter are producing first-rate science at the Intensity and Cosmic Frontiers. Plans for future importance of maintaining detector and accelerator R&D for future projects in difficult budget times

Quigg, Chris

171

Cosmic antifriction and accelerated expansion  

Science Journals Connector (OSTI)

We explain an accelerated expansion of the present Universe, suggested from observations of supernovae of type Ia at high redshift, by introducing an antifrictional force that is self-consistently exerted on the particles of the cosmic substratum. Cosmic antifriction, which is intimately related to particle production, is shown to give rise to an effective negative pressure of the cosmic medium. While other explanations for an accelerated expansion (cosmological constant, quintessence) introduce a component of dark energy in addition to standard cold dark matter (CDM) we resort to a phenomenological one-component model of CDM with internal self-interactions. We demonstrate how the dynamics of the cold dark matter model with a cosmological constant may be recovered as a special case of cosmic antifriction. We discuss the connection with two-component models and obtain an attractor behavior for the ratio of the energy densities of both components which provides a possible phenomenological solution to the coincidence problem.

Winfried Zimdahl; Dominik J. Schwarz; Alexander B. Balakin; Diego Pavn

2001-08-03T23:59:59.000Z

172

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

173

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

174

Cosmic Rays at the Knee  

E-Print Network (OSTI)

Several kinds of measurements are combined in an attempt to obtain a consistent estimate of the spectrum and composition of the primary cosmic radiation through the knee region. Assuming that the knee is a signal of the high-energy end of a galactic cosmic-ray population, I discuss possible signatures of a transition to an extra-galactic population and how they might be detected.

Thomas K. Gaisser

2006-08-25T23:59:59.000Z

175

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

176

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

177

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

178

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

179

Exploring Frontiers in Kinetics and Mechanisms of Geochemical Processes at the Mineral/Water Interface  

E-Print Network (OSTI)

Exploring Frontiers in Kinetics and Mechanisms of Geochemical Processes at the Mineral in the Earth's Critical Zone is the kinetics. The timescales for geochemical processes range from milliseconds geochemical processes including surface complexation, mineral transformations, and oxidation

Sparks, Donald L.

180

SMA and MACD combinations for stock investment decisions in frontier markets: evidence from Dubai financial market  

Science Journals Connector (OSTI)

One of the most challenging financial decisions is when to buy and sell stocks. Frontier markets offer high profit opportunities but also have high risk. Consequently, technical analysis is used to assist in properly timing entry and exit points from stock trades. Previous research presented applications of technical analysis in developed and emerging markets since they, unlike frontier markets, exist in an environment of political stability, regulations, and liquidity. This paper shows how trade signals generated from Simple Moving Average (SMA) confirmed by Moving Average Convergence Divergence (MACD) can be used to minimise trading risk in frontier markets such as Dubai Financial Market (DFM). The results show that the standard time-periods for SMA and MACD do not apply well to frontier markets and that trade signals generated from SMA and confirmed by signals generated from medium to long-term MACD or vice versa result in excellent hit ratios.

Hazim El-Baz; Ibrahim Al Awadhi; Assia Lasfer

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.


181

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 components. Applications of these techniques to assess metal and organic chemical sorption/release, natural widely employed to provide an indirect assessment ofchemical speciation and association ofcontaminants

Sparks, Donald L.

182

LALP-07-023 Spring 2007 he opportunity to explore new scientific frontiers awaits  

E-Print Network (OSTI)

LALP-07-023 Spring 2007 T he opportunity to explore new scientific frontiers awaits users, with forces so far beyond the material strengths that the simplistic coil is destroyed with each pulse

183

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

184

BAYESIAN INFERENCE OF POLARIZED COSMIC MICROWAVE BACKGROUND POWER SPECTRA FROM INTERFEROMETRIC DATA  

SciTech Connect

Detection of B-mode polarization of the cosmic microwave background (CMB) radiation is one of the frontiers of observational cosmology. Because they are an order of magnitude fainter than E-modes, it is quite a challenge to detect B-modes. Having more manageable systematics, interferometers prove to have a substantial advantage over imagers in detecting such faint signals. Here, we present a method for Bayesian inference of power spectra and signal reconstruction from interferometric data of the CMB polarization signal by using the technique of Gibbs sampling. We demonstrate the validity of the method in the flat-sky approximation for a simulation of an interferometric observation on a finite patch with incomplete uv-plane coverage, a finite beam size, and a realistic noise model. With a computational complexity of O(n {sup 3/2}), n being the data size, Gibbs sampling provides an efficient method for analyzing upcoming cosmology observations.

Karakci, Ata; Korotkov, Andrei; Tucker, Gregory S. [Department of Physics, Brown University, 182 Hope Street, Providence, RI 02912 (United States); Sutter, P. M.; Wandelt, Benjamin D. [Department of Physics, 1110 W. Green Street, University of Illinois at Urbana-Champaign, Urbana, IL 61801 (United States); Zhang, Le; Timbie, Peter [Department of Physics, University of Wisconsin, Madison, WI 53706 (United States); Bunn, Emory F., E-mail: ata_karakci@brown.edu [Physics Department, University of Richmond, Richmond, VA 23173 (United States)

2013-01-15T23:59:59.000Z

185

Cosmic String Loop Microlensing  

E-Print Network (OSTI)

Cosmic superstring loops within the galaxy microlens background point sources lying close to the observer-string line of sight. For suitable alignments, multiple paths coexist and the (achromatic) flux enhancement is a factor of two. We explore this unique type of lensing by numerically solving for geodesics that extend from source to observer as they pass near an oscillating string. We characterize the duration of the flux doubling and the scale of the image splitting. We probe and confirm the existence of a variety of fundamental effects predicted from previous analyses of the static infinite straight string: the deficit angle, the Kaiser-Stebbins effect, and the scale of the impact parameter required to produce microlensing. Our quantitative results for dynamical loops vary by O(1) factors with respect to estimates based on infinite straight strings for a given impact parameter. A number of new features are identified in the computed microlensing solutions. Our results suggest that optical microlensing can offer a new and potentially powerful methodology for searches for superstring loop relics of the inflationary era.

Jolyon K. Bloomfield; David F. Chernoff

2013-11-27T23:59:59.000Z

186

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)  

ScienceCinema (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

2011-11-03T23:59:59.000Z

187

Lattice QCD  

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

Lattice QCD Lattice QCD Understanding discoveries at the Energy, Intensity, and Cosmic Frontiers Get Expertise Rajan Gupta (505) 667-7664 Email Bruce Carlsten (505) 667-5657 Email...

188

Lunar/Solar effects on Cosmic Rays  

E-Print Network (OSTI)

Lunar/Solar effects on Cosmic Rays By: Sophia Bauer & Jenna Valdez #12;Introduction When cosmic, California." Moon Phase Calendar for Santa Cruz, California. N.p., n.d. Web. 02 Aug. 2012.

California at Santa Cruz, University of

189

Light-Material Interactions in Energy Conversion - Energy Frontier...  

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

Waals interactions, without the use of applied pressure or precision alignment stages. Light passing through the mask generates a distribution of intensity that can expose a layer...

190

COSMIC-RAY MUON TOMOGRAPHY AND ITS APPLICATION TO THE DETECTION OF HIGH-Z MATERIALS  

E-Print Network (OSTI)

. The mean energy of the muons at the ground is about 4 GeV. The integral 1 #12;intensity of vertical muons change their directions due to the multiple scattering, lose their energy and finally get stopped. A muonCOSMIC-RAY MUON TOMOGRAPHY AND ITS APPLICATION TO THE DETECTION OF HIGH-Z MATERIALS Konstantin

Kurien, Susan

191

Cosmic Ray Origins: An Introduction  

E-Print Network (OSTI)

Physicists have pondered the origin of cosmic rays for over a hundred years. However the last few years have seen an upsurge in the observation, progress in the theory and a genuine increase in the importance attached to the topic due to its intimate connection to the indirect detection of evidence for dark matter. The intent of this talk is to set the stage for the meeting by reviewing some of the basic features of the entire cosmic ray spectrum from GeV to ZeV energy and some of the models that have been developed. The connection will also be made to recent developments in understanding general astrophysical particle acceleration in pulsar wind nebulae, relativistic jets and gamma ray bursts. The prospects for future discoveries, which may elucidate the origin of cosmic rays, are bright.

Blandford, Roger; Yuan, Yajie

2014-01-01T23:59:59.000Z

192

Production of Low-Energy Cosmic-Ray Electrons  

Science Journals Connector (OSTI)

The production of cosmic-ray electrons of characteristically low energies is investigated. Secondary sources, other than that of meson decay, are considered, and constraints are placed on both secondary and primary sources. (1) Calculations are made of the intensity of low-energy knock-on and beta-decay electrons which are secondary to cosmic-ray interactions. In particular, knock-on production is calculated in the 100-KeV to 50-BeV kinetic-energy interval. Interstellar losses due to ionization, leakage from the galaxy, and synchrotron, bremsstrahlung, and inverse Compton effects are considered, as well as those due to plasma excitation, the red shift and synchrotron, bremsstrahlung, and inverse Compton effects in the intergalactic medium. The intensity of low-energy relativistic electrons from these sources is not negligible compared with the low energy ????e intensity, but it is shown not to account for the observed interplanetary electron intensity. (2) Energy inputs to the injected secondary electrons by a possible solar electric field of low magnitude and by a possible galactic Fermi acceleration are investigated. It is shown that at least one such input is necessary if the observed low-energy interplanetary electron intensity is to be attributed to secondary production alone. A heliocentric field which does allow for a fit to the low-energy data cannot, however, account for the high-energy BeV electrons found to be in excess of those from ????e production. The Fermi acceleration shown to be necessary to provide a fit is greater than that usually postulated for cosmic-ray protons, and also requires that the ratio of escape losses to acceleration ?? be much smaller than is usually assumed for protons. This distinction is acceptable only if one postulates a significant difference between interstellar proton and electron propagation. (3) The observation that the velocity spectrum of electrons in the energy-per-unit-mass region of 7-25 closely approximates that of the cosmic-ray protons, and the necessity of constraints on the secondary-electron hypothesis outlined above, suggest that most of the low-energy electrons are of primary origin. The similarity between this conclusion and the conclusion (based on the measurement of the charge ratio of electrons) that the higher energy electrons are mostly primary is discussed.

P. B. Abraham; K. A. Brunstein; T. L. Cline

1966-10-28T23:59:59.000Z

193

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

194

Cosmic Particle Acceleration: Basic Issues  

E-Print Network (OSTI)

Cosmic-rays are ubiquitous, but their origins are surprisingly difficult to understand. A review is presented of some of the basic issues common to cosmic particle accelerators and arguments leading to the likely importance of diffusive shock acceleration as a general explanation. The basic theory of diffusive shock acceleration is outlined, followed by a discussion of some of the key issues that still prevent us from a full understanding of its outcomes. Some recent insights are mentioned at the end that may help direct ultimate resolution of our uncertainties.

T. W. Jones

2000-12-22T23:59:59.000Z

195

Mid-continent rift system: a frontier hydrocarbon province  

SciTech Connect

The Mid-continent rift system can be traced by the Mid-continent geophysical anomaly (MGA) from the surface exposure of the Keweenawan Supergroup in the Lake Superior basin southwest in the subsurface through Wisconsin, Minnesota, Iowa, Nebraska, and Kansas. Outcrop and well penetrations of the late rift Keweenawan sedimentary rocks reveal sediments reflecting a characteristic early continental rift clastic sequence, including alluvial fans, deep organic-rich basins, and prograding fluvial plains. Sedimentary basins where these early rift sediments are preserved can be located by upward continuation of the aeromagnetic profiles across the rift trend and by gravity models. Studies of analog continental rifts and aulacogens show that these gravity models should incorporate (1) a deep mafic rift pillow body to create the narrow gravity high of the MGA, and (2) anomalously thick crust to account for the more regional gravity low. Preserved accumulations of rift clastics in central rift positions can then be modeled to explain the small scale notches which are found within the narrow gravity high. Indigenous oil in Keweenawan sediments in the outcrop area and coaly partings in the subsurface penetrations of the Keweenawan clastics support the analogy between these rift sediments and the exceptionally organic-rich sediments of the East African rift. COCORP data across the rift trend in Kansas show layered deep reflectors and large structures. There is demonstrable source, reservoir, and trap potential within the Keweenawan trend, making the Mid-Continent rift system a frontier hydrocarbon province.

Lee, C.K.; Kerr, S.D. Jr.

1984-04-01T23:59:59.000Z

196

Mid-Continent rift system: a frontier hydrocarbon province  

SciTech Connect

The Mid-Continent rift system can be traced by the Mid-Continent geophysical anomaly (MGA) from the surface exposure of the Keweenawan Supergroup in the Lake Superior basin southwest in the subsurface through Wisconsin, Minnesota, Iowa, Nebraska, and Kansas. Outcrop and well penetrations of the late rift Keweenawan sedimentary rocks reveal sediments reflecting a characteristic early continental rift clastic sequence, including alluvial fans, deep organic-rich basins, and prograding fluvial plains. Sedimentary basins where these early rift sediments are preserved can be located by upward continuation of the aeromagnetic profiles across the rift trend and by gravity models. Studies of analog continental rifts and aulacogens show that these gravity models should incorporate (1) a deep mafic rift pillow body to create the narrow gravity high of the MGA, and (2) anomalously thick crust to account for the more regional gravity low. Preserved accumulations of rift clastics in central rift positions can then be modeled to explain the small scale notches which are found within the narrow gravity high. Indigenous oil in Keweenawan sediments in the outcrop area and coaly partings in the subsurface penetrations of the Keweenawan clastics support the analogy between these rift sediments and the exceptionally organic-rich sediments of the East African rift. COCORP data across the rift trend in Kansas show layered deep reflectors and large structures. There is demonstrable source, reservoir, and trap potential within the Keweenawan trend, making the Mid-Continent rift system a frontier hydrocarbon province.

Lee, C.K.; Kerr, S.D. Jr.

1984-04-01T23:59:59.000Z

197

Ohio State's researchers to collaborate on three new Ohio Third Frontier photovoltaics grants Ohio State's Institute for Materials Research (IMR) is the central collaborator on three Ohio Third Frontier Photovoltaics  

E-Print Network (OSTI)

Ohio State's researchers to collaborate on three new Ohio Third Frontier photovoltaics grants Ohio Photovoltaics Program (PVP) projects recommended for funding by the Ohio Third Frontier Commission. The goal of the PVP is to accelerate the development and growth of the photovoltaics industry in Ohio by supporting

198

The Physics of Cosmic Acceleration  

E-Print Network (OSTI)

by Annual Reviews. All rights reserved 0163-8998/09/1123-0397$20.00 Key Words cosmology, dark energy · Our comprehensive search FurtherANNUAL REVIEWS #12;Dark energy: a negative-pressure fluid comprising, particle theory, gravitational theory Abstract The discovery that the cosmic expansion is accelerating has

Weijgaert, Rien van de

199

On the trailof COSMIC BULLETS  

E-Print Network (OSTI)

|volume04|issue08/09|oct/nov07 17 Argentina's Pampa Amarilla is a rather remote place, a dry plain, an unusually powerful cosmic ray strikes the Earth's atmosphere with almost as much energy as a bullet. Fortunately, such a projectile is no danger to human life. Entering the atmosphere, it loses energy

200

Ultra High Energy Cosmic Rays  

Science Journals Connector (OSTI)

We discuss briefly the phenomenon of the Ultra High Energy Cosmic Rays (UHECR) particles of energy approaching and exceeding 1011 GeV. The world experimental statistics contains a small number of events but their existence is a puzzle. Its solution may lead to exciting discoveries in high energy particle astrophysics as well as in particle physics and astronomy.

Todor Stanev

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.


201

Ultra High Energy Cosmic Rays  

Science Journals Connector (OSTI)

......tral data at energies above 1 EeV (1018eV...from the AGASA project, are very suggestive...since these low energy cosmic rays have...the outflowing solar wind plasma and...it does on the energy limit set by the solar wind. Since there......

Roger Clay

2003-05-01T23:59:59.000Z

202

Cosmic-ray driven winds  

E-Print Network (OSTI)

The theory of Galactic Winds, driven by the cosmic-ray pressure gradient, is reviewed both on the magnetohydrodynamic and on the kinetic level. In this picture the magnetic field of the Galaxy above the dense gas disk is assumed to have a flux tube geometry, the flux tubes rising locally perpendicular out of the disk to become radially directed at large distances, with the cosmic-ray sources located deep within the Galactic disk. At least above the gas disk, the magnetic fluctuations which resonantly scatter the cosmic rays are selfconsistently excited as Alf{`e}n waves by the escaping cosmic rays. The fluctuation amplitudes remain finite through nonlinear wave dissipation. The spatially increasing speed of the resulting outflow results in a diffusion-convection boundary whose position depends on particle momentum. It replaces the escape boundary of static diffusion models. New effects like overall Galactic mass and angular momentum loss as well as gas heating beyond the disk appear. Also particle re-accelera...

Vlk, Heinrich J

2014-01-01T23:59:59.000Z

203

Temporal and energy behavior of cosmic ray fluxes in the periods of low solar activity  

E-Print Network (OSTI)

Modulation of galactic cosmic ray intensity is governed by several mechanisms including diffusion, convection, adiabatic energy losses and drift. Relative roles of these factors change in the course of an 11-year solar cycle. That can result in the changes in the energy dependence of the 11-year cosmic ray modulation. The minimum between the solar cycles 23 and 24 was extremely deep and long-lasting which led to the record high cosmic ray fluxes low-energy particles dominating. This was a signature of unusually soft energy spectrum of the cosmic rays. In this work we examine the energy dependence of the 11-year modulation during the last three solar cycles and argue that a soft energy spectrum was observed in the minimum of each cycle however only for particles below of energy around 10 GeV. From mid 1980s the energy dependence of cosmic rays became softer from minimum to minimum of solar activity. The work is based on the cosmic ray data of the spacecraft, balloon-borne and the ground-based observations.

Bazilevskaya, G A; Krainev, M B; Makhmutov, V S; Svirzhevskaya, A K; Svirzhevsky, N S

2014-01-01T23:59:59.000Z

204

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

205

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

206

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.

207

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

208

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

209

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

2005-03-08T23:59:59.000Z

210

The Cosmic Near Infrared Background: Remnant Light from Early Stars  

E-Print Network (OSTI)

The redshifted ultraviolet light from early stars at z ~ 10 contributes to the cosmic near infrared background. We present detailed calculations of its spectrum with various assumptions about metallicity and mass spectrum of early stars. We show that if the near infrared background has a stellar origin, metal-free stars are not the only explanation of the excess near infrared background; stars with metals (e.g. Z=1/50 Z_sun) can produce the same amount of background intensity as the metal-free stars. We quantitatively show that the predicted average intensity at 1-2 microns is essentially determined by the efficiency of nuclear burning in stars, which is not very sensitive to metallicity. We predict \

Elizabeth Fernandez; Eiichiro Komatsu

2005-08-08T23:59:59.000Z

211

Electromagnetic field and cosmic censorship  

E-Print Network (OSTI)

We construct a gedanken experiment in which an extremal Kerr black hole interacts with a test electromagnetic field. Using Teukolsky's solutions for electromagnetic perturbations in Kerr spacetime, and the conservation laws imposed by the energy momentum tensor of the electromagnetic field and the Killing vectors of the spacetime, we prove that this interaction cannot convert the black hole into a naked singularity, thus cosmic censorship conjecture is not violated in this case.

Koray Dzta?

2014-04-09T23:59:59.000Z

212

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

213

Gravitational waves versus cosmic strings  

Science Journals Connector (OSTI)

The equation which governs the temporal evolution of a gravitational wave (GW) in curved space-time can be treated as the Schrodinger equation for a particle moving in the presence of an effective potential. When GWs propagate in an expanding Universe with constant effective potential, there is a critical value (kc) of the comoving wave-number which discriminates the metric perturbations into oscillating (k > kc) and non-oscillating (k kc) modes. The effective potential is reduced to a non-vanishing constant in a cosmological model which is driven by a two-component fluid, consisting of radiation (dominant) and cosmic strings (subdominant). However, the cosmological evolution (gradually) results in the scaling of any long-cosmic-string network and, therefore, after some time (??) the Universe enters in the pure-radiation epoch. The evolution of the non-oscillatory GW modes during ??, results in the distortion of the low-frequency part of the stochastic GW power-spectrum, which, therefore, departs from scale invariance (anticipated in the pure-radiation case). As regards the corresponding high-frequency part (which is determined by the evolution of the oscillating modes), we find that the presence of cosmic strings gives rise to the quantum-gravitational creation of gravitons, leading to the amplification of the GW signal by (almost) two orders of magnitude.

Kostas Kleidis

2009-01-01T23:59:59.000Z

214

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  

ScienceCinema (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

2011-11-02T23:59:59.000Z

215

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

SciTech Connect

'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) [Director, Center for Excitonics; Center for Excitonics Staff

2011-05-01T23:59:59.000Z

216

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)  

ScienceCinema (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

2011-11-02T23:59:59.000Z

217

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

ScienceCinema (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

2011-11-02T23:59:59.000Z

218

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)  

ScienceCinema (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

2011-11-02T23:59:59.000Z

219

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)  

ScienceCinema (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

2011-11-02T23:59:59.000Z

220

Cloud chamber visualization of primary cosmic rays  

SciTech Connect

From 1948 until 1963, cloud chambers were carried to the top of the atmosphere by balloons. From these flights, which were begun by Edward P. Ney at the University of Minnesota, came the following results: discovery of heavy cosmic ray nuclei, development of scintillation and cherenkov detectors, discovery of cosmic ray electrons, and studies of solar proton events. The history of that era is illustrated here by cloud chamber photographs of primary cosmic rays.

Earl, James A. [Department of Astronomy, University of Maryland, College Park MD (United States)

2013-02-07T23:59:59.000Z

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

NONLINEAR AERODYNAMIC ANALYSIS OF BRIDGES UNDER TURBULENT WINDS: THE NEW FRONTIER IN BRIDGE  

E-Print Network (OSTI)

NONLINEAR AERODYNAMIC ANALYSIS OF BRIDGES UNDER TURBULENT WINDS: THE NEW FRONTIER IN BRIDGE AERODYNAMICS Xinzhong Chen , Ahsan Kareem and Fred L. Haan, Jr. ¡ Department of Civil Engineering. These approaches are limited to linear structures in which nonlinearities in aerodynamic forces are ignored

Kareem, Ahsan

222

Exploring the Frontiers of Burning Science Dale Meade and the FIRE Team  

E-Print Network (OSTI)

Exploring the Frontiers of Burning Science Dale Meade and the FIRE Team ITC-12 / APFA '01 Meeting, and it produces negligible nuclear waste or pollutants." What should we do to be ready? By end of January conduct the base fusion sciences program 2. Directs DOE to submit a plan for construction of a U.S. Burning Plasma

223

Nanoscience This course explores the frontiers of science on the nanoscale. Many developing 21st  

E-Print Network (OSTI)

Nanoscience MSc/PgDip This course explores the frontiers of science on the nanoscale. Many and behaviours of systems in this submicrometrescale size domain. The multidisciplinary nature of nanoscience. The projects take place primarily in research labs associated with nanoscience located in the University

Strathclyde, University of

224

The Final Frontier for Humanity by Dr L S Chan, Department of Earth Sciences  

E-Print Network (OSTI)

The Final Frontier for Humanity by Dr L S Chan, Department of Earth Sciences "Fossil fuels supply treatment, air and water pollution, species extinctions, climatic calamities, sea level rises solutions for any of these problems yet. Development requires resources and generates wastes. Earth

Jiao, Jiu Jimmy

225

Vision Statement for Plant Physiology Comparative Plant Genomics. Frontiers and Prospects  

E-Print Network (OSTI)

Vision Statement for Plant Physiology Comparative Plant Genomics. Frontiers and Prospects Ana L function and evolution at various levels of biological organiza- tion. The availability of whole-genome sequences as well as other genomic resources (e.g. microarray meth- ods, expressed sequence tag [EST

Purugganan, Michael D.

226

Resource Letter FNP-1: Frontiers of nuclear physics G. F. Bertscha)  

E-Print Network (OSTI)

Resource Letter FNP-1: Frontiers of nuclear physics G. F. Bertscha) Department of Physics activities in nuclear physics and also a guide for finding useful nuclear data. The major areas included, and nuclear instrumentation. © 2004 American Association of Physics Teachers. DOI: 10.1119/1.1763174 I

Bertsch George F.

227

The ATLAS Detector at the LHC Results from the New Energy Frontier  

E-Print Network (OSTI)

The ATLAS Detector at the LHC Results from the New Energy Frontier Cristina Oropeza Barrera A Toroidal LHC ApparatuS ATLAS is the largest particle detector ever built! Integrated by four mainS ATLAS is a general-purpose detector. Physics goals: · Re-discover the Standard Model: · Minimum Bias

Greenaway, Alan

228

Duty-Cycling Buildings Aggressively: The Next Frontier in HVAC Control  

E-Print Network (OSTI)

Duty-Cycling Buildings Aggressively: The Next Frontier in HVAC Control Yuvraj Agarwal, Bharathan the dominant energy consumer is the HVAC system. Despite this fact, in most buildings the HVAC system is run sensing to guide the operation of a building HVAC system. We show how we can enable aggressive duty

Simunic, Tajana

229

FRONTIERS ARTICLE Fundamentals of energy transport, energy conversion, and thermal properties  

E-Print Network (OSTI)

FRONTIERS ARTICLE Fundamentals of energy transport, energy conversion, and thermal properties, thermoelectrics, and photovoltaics. However, energy transport and conversion, at the organic­inorganic interface and as an energy conversion technology. Aviram and Ratner's revolutionary suggestion that molecules could behave

Malen, Jonathan A.

230

Advancing the Frontiers in Nanocatalysis, Biointerfaces, and Renewable Energy Conversion by Innovations of Surface Techniques  

Science Journals Connector (OSTI)

Advancing the Frontiers in Nanocatalysis, Biointerfaces, and Renewable Energy Conversion by Innovations of Surface Techniques ... (80-86) These energetic electrons that are not in thermal equilibrium with the metal atoms are called hot electrons. ... The activation energies are 22-33 kcal/mol, close to the desorption energy of CO from these surfaces. ...

Gabor A. Somorjai; Heinz Frei; Jeong Y. Park

2009-11-04T23:59:59.000Z

231

Byzantine naval power and trade: the collapse of the western frontier  

E-Print Network (OSTI)

In the eleventh century A.D., the Byzantine Empire witnessed a number of military and political disasters. One of the most significant of these was the collapse of the western frontier and final loss of southern Italy in 1071. However...

Scafuri, Michael Phillip

2002-01-01T23:59:59.000Z

232

Frontiers in Public Health Services and Systems Research Volume 1 | Number 1 Article 6  

E-Print Network (OSTI)

improvement plans. Since these activities are fundamental aspects of accreditation and health reformFrontiers in Public Health Services and Systems Research Volume 1 | Number 1 Article 6 4-17-2012 Patterns of Interaction Among Local Public Health Officials and the Adoption of Recommended Practices

Sadeh, Norman M.

233

Apply: Building Energy Efficiency Frontiers and Incubator Technologies (BENEFIT)- 2014 (DE-FOA-0001027)  

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

Closed Total DOE Funding: $14 million Deadline: April 21, 2014 This funding opportunity intends to advance innovative, energy-efficient technologies, approaches, and design tools for commercial and/or residential buildings. The funding opportunity covers two focus areas, Incubators and Frontiers (Innovations).

234

Apply: Building Energy Efficiency Frontiers and Innovation Technologies (BENEFIT)- 2015 Funding Opportunity Announcement  

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

Deadline for Concept Papers: November 10, 2014, 5:00 PM ET This Building Energy Efficiency Frontiers and Innovations Technologies (BENEFIT) 2015 FOA contributes to advancement in two core technological areas: non-vapor compression HVAC technologies and advanced vapor compression HVAC technologies.

235

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

236

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

237

Probing Fukushima with cosmic rays should help speed cleanup...  

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

Probing Fukushima with cosmic rays Probing Fukushima with cosmic rays should help speed cleanup of damaged plant The initiative could reduce the time required to clean up the...

238

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

239

Frontiers for Discovery in High Energy Density Physics  

SciTech Connect

The report is intended to identify the compelling research opportunities of high intellectual value in high energy density physics. The opportunities for discovery include the broad scope of this highly interdisciplinary field that spans a wide range of physics areas including plasma physics, laser and particle beam physics, nuclear physics, astrophysics, atomic and molecular physics, materials science and condensed matter physics, intense radiation-matter interaction physics, fluid dynamics, and magnetohydrodynamics

Davidson, R. C.; Katsouleas, T.; Arons, J.; Baring, M.; Deeney, C.; Di Mauro, L.; Ditmire, T.; Falcone, R.; Hammer, D.; Hill, W.; Jacak, B.; Joshi, C.; Lamb, F.; Lee, R.; Logan, B. G.; Melissinos, A.; Meyerhofer, D.; Mori, W.; Murnane, M.; Remington, B.; Rosner, R.; Schneider, D.; Silvera, I.; Stone, J.; Wilde, B.; Zajc. W.

2004-07-20T23:59:59.000Z

240

Measurements of the energy spectrum of cosmic-ray muons at sea-level with emulsion chambers  

Science Journals Connector (OSTI)

The energy spectrum of cosmic-ray muons at sea-level has been measured in the energy range of 1 TeV to 10 TeV ... tons of lead/year. On the vertical muon intensity, it is shown that the index ... law. The zenith ...

K. Mizutani; A. Misaki; T. Shirai; Z. Watanabe; M. Akashi

1978-01-21T23:59:59.000Z

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

Magnetic Moment of Electrons near Cosmic Strings  

E-Print Network (OSTI)

We study the effect of background geometry generated by a thin cosmic string on the anomalous magnetic moment of the electron. We find that the magnitude of the quantum correction to the magnetic moment depends on the distance from the cosmic string as well as on the deficit angle.

Takuya Maki; Kiyoshi Shiraishi

2014-01-27T23:59:59.000Z

242

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

243

Cosmic Ray Physics with ACORDE at LHC  

E-Print Network (OSTI)

The use of large underground high-energy physics experiments, for comic ray studies, have been used, in the past, at CERN, in order to measure, precisely, the inclusive cosmic ray flux in the energy range from 2x10^10 - 2x10^12 eV. ACORDE, ALICE Cosmic Rays DEtector, will act as Level 0 cosmic ray trigger and, together with other ALICE apparatus, will provide precise information on cosmic rays with primary energies around 10^15 - 10^17 eV. This paper reviews the main detector features, the present status, commissioning and integration with other apparatus. Finally, we discuss the ACORDE-ALICE cosmic ray physics program.

C. Pagliarone; A. Fernandez-Tellez

2007-09-19T23:59:59.000Z

244

Further Experiments on the Uniformity of Distribution of the Cosmic Radiation  

Science Journals Connector (OSTI)

More careful and prolonged observations on the small, daily variation before reported in the measured intensities of the cosmic rays, the new observations being made under such conditions as to eliminate the possibility of a slight temperature effect suggested by Bowen and Millikan's recent explanation of ionization-pressure relations in high-pressure electroscopes, yield the definite result that within the limits of the author's present observational uncertainty which is of the order of a third of a percent, the sun has no direct influence on cosmic-ray intensities. New evidence is presented that if observed and apparently systematic variations of the order of a third of a percent are in fact real they are best interpreted as the result of small changes in the blanketing effect of the earth's atmosphere due to air currents.

Robert A. Millikan

1932-02-01T23:59:59.000Z

245

Energy Intensity Strategy  

E-Print Network (OSTI)

Our presentation will cover how we began the journey of conserving energy at our facility. Well discuss a basic layout of our energy intensity plan and the impact our team has had on the process, what tools were using, what goals have been...

Rappolee, D.; Shaw, J.

2008-01-01T23:59:59.000Z

246

The Cosmic Equation of State  

E-Print Network (OSTI)

The cosmic spacetime is often described in terms of the FRW metric, though the adoption of this elegant and convenient solution to Einstein's equations does not tell us much about the equation of state, p=w rho, in terms of the total energy density rho and pressure p of the cosmic fluid. LCDM and the R_h=ct Universe are both FRW cosmologies that partition rho into (at least) three components, matter rho_m, radiation rho_r, and a poorly understood dark energy rho_de, though the latter goes one step further by also invoking the constraint w=-1/3. This condition is required by the simultaneous application of the Cosmological principle and Weyl's postulate. Model selection tools in one-on-one comparisons favor R_h=ct with a likelihood of ~90% versus only ~10% for LCDM. Nonetheless, the predictions of LCDM often come quite close to those of R_h=ct, suggesting that its parameters are optimized to mimic the w=-1/3 equation of state. In this paper, we demonstrate that the equation of state in R_h=ct helps us to under...

Melia, Fulvio

2014-01-01T23:59:59.000Z

247

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

ScienceCinema (OSTI)

'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

2011-11-02T23:59:59.000Z

248

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

SciTech Connect

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

2011-05-01T23:59:59.000Z

249

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

ScienceCinema (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

2011-11-02T23:59:59.000Z

250

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

251

The intensity of motivation  

E-Print Network (OSTI)

rearranged before they were repeated in reverse sequence. Electrocardiographic T-wave amplitude (TWA) and changes were monitored during a 15-sec anticipatory phase, as well as during each 15-second mental manipulation phase. (This ensured that the measures..., and the subject was surreptitiously observed. The high-self-esteem subjects were observed to do more practice www.annualreviews.org/aronline Annual Reviews INTENSITY OF MOTIVATION 121 problems for the difficult- than for the easy-to-please experimenter...

Brehm, Jack W.; Self, E. A.

1989-01-01T23:59:59.000Z

252

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

253

Gauging the cosmic microwave background  

E-Print Network (OSTI)

We provide a new derivation of the anisotropies of the cosmic microwave background (CMB), and find an exact expression that can be readily expanded perturbatively. Close attention is paid to gauge issues, with the motivation to examine the effect of super-Hubble modes on the CMB. We calculate a transfer function that encodes the behaviour of the dipole, and examine its long-wavelength behaviour. We show that contributions to the dipole from adiabatic super-Hubble modes are strongly suppressed, even in the presence of a cosmological constant, contrary to claims in the literature. We also introduce a naturally defined CMB monopole, which exhibits closely analogous long-wavelength behaviour. We discuss the geometrical origin of this super-Hubble suppression, pointing out that it is a simple reflection of adiabaticity, and hence argue that it will occur regardless of the matter content.

J. P. Zibin; Douglas Scott

2008-12-21T23:59:59.000Z

254

Scaling of cosmic string loops  

E-Print Network (OSTI)

We study the spectrum of loops as a part of a complete network of cosmic strings in flat space-time. After a long transient regime, characterized by production of small loops at the scale of the initial conditions, it appears that a true scaling regime takes over. In the final regime the characteristic size of loops scales as $0.1 t$, and the production rate of small loops goes as $l^{-1.63}$. In the expanding universe, we expect similar behavior with perhaps a less negative index. For such indices, the distribution of loops existing at any given time goes as $l^{-5/2}$ in the radiation era and $l^{-2}$ in the matter era.

Vanchurin, V; Vilenkin, A; Olum, Ken D.; Vanchurin, Vitaly; Vilenkin, Alexander

2006-01-01T23:59:59.000Z

255

The Cosmic Equation of State  

E-Print Network (OSTI)

The cosmic spacetime is often described in terms of the FRW metric, though the adoption of this elegant and convenient solution to Einstein's equations does not tell us much about the equation of state, p=w rho, in terms of the total energy density rho and pressure p of the cosmic fluid. LCDM and the R_h=ct Universe are both FRW cosmologies that partition rho into (at least) three components, matter rho_m, radiation rho_r, and a poorly understood dark energy rho_de, though the latter goes one step further by also invoking the constraint w=-1/3. This condition is required by the simultaneous application of the Cosmological principle and Weyl's postulate. Model selection tools in one-on-one comparisons favor R_h=ct with a likelihood of ~90% versus only ~10% for LCDM. Nonetheless, the predictions of LCDM often come quite close to those of R_h=ct, suggesting that its parameters are optimized to mimic the w=-1/3 equation of state. In this paper, we demonstrate that the equation of state in R_h=ct helps us to understand why the optimized fraction Omega_m=rho_m/rho in LCDM must be ~0.27, an otherwise seemingly random variable. We show that when one forces LCDM to satisfy the equation of state w=(rho_r/3-rho_de)/rho, the value of the Hubble radius today, c/H_0, can equal its measured value ct_0 only with Omega_m~0.27 when the equation of state for dark energy is w_de=-1. This peculiar value of Omega_m therefore appears to be a direct consequence of trying to fit the data with the equation of state w=(rho_r/3-rho_de)/rho in a Universe whose principal constraint is instead R_h=ct or, equivalently, w=-1/3.

Fulvio Melia

2014-11-21T23:59:59.000Z

256

E-Print Network 3.0 - absolute cosmic distance Sample Search...  

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

the COSMIC FORMOSAT-3 Mission Bill Kuo UCAR COSMIC Project FORMOSAT-3 12... ;COSMIC (Constellation Observing System for Meteorology, Ionosphere and Climate) 6 Satellites was...

257

The beginning of cosmic ray astronomy  

E-Print Network (OSTI)

We discuss the anisotropic arrival directions of the ultra high energy cosmic rays detected by Auger which I consider one of the biggest discoverie in astrophysics during the last year.

Todor Stanev

2008-08-08T23:59:59.000Z

258

Cosmic-ray muons at ultrahigh energies  

Science Journals Connector (OSTI)

Fluxes of cosmic-ray muons were estimated over the energy range extending up to 1010 GeV. Data on the production of pions; kaons; ?, ??, ?, ?, and ? mesons; charmed particles; and J/?...mesons from accelerator ex...

L. V. Volkova

2011-02-01T23:59:59.000Z

259

Annual modulation of cosmic relic neutrinos  

E-Print Network (OSTI)

The cosmic neutrino background (C?B), produced about one second after the big bang, permeates the Universe today. New technological advancements make neutrino capture on beta-decaying nuclei (NCB) a clear path forward ...

Safdi, Benjamin R.

260

Terrestrial Effects of High Energy Cosmic Rays  

E-Print Network (OSTI)

On geological timescales, the Earth is likely to be exposed to higher than the usual flux of high energy cosmic rays (HECRs) from astrophysical sources such as nearby supernovae, gamma ray bursts or by galactic shocks. ...

Atri, Dimitra

2011-04-26T23:59:59.000Z

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.


261

Yakov Zeldovich and the Cosmic Web Paradigm  

E-Print Network (OSTI)

I discuss the formation of the modern cosmological paradigm. In more detail I describe the early study of dark matter and cosmic web and the role of Yakov Zeldovich in the formation of the present concepts on these subjects.

Einasto, Jaan

2014-01-01T23:59:59.000Z

262

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

263

Preliminary Results from the Cosmic Background Imager  

E-Print Network (OSTI)

The Cosmic Background Imager (CBI) is a 13-element interferometer designed to image intrinsic anisotropies in the cosmic microwave background (CMB) on arcminute scales. A review of the capabilities of the instrument is presented, together with a discussion of observations which have been taken over the past 9 months from the Atacama desert of Chile. We present preliminary high-resolution mosaiced images of the CMB obtained from recent CBI data and discuss topics which the CBI will address in the near future.

B. S. Mason; J. K. Cartwright; S. Padin; T. J. Pearson; A. C. S. Readhead; M. Shepherd; J. Sievers; P. Udomprasert

2001-01-11T23:59:59.000Z

264

Influence of Cosmic Rays on Earth's Climate  

Science Journals Connector (OSTI)

During the last solar cycle Earth's cloud cover underwent a modulation more closely in phase with the galactic cosmic ray flux than with other solar activity parameters. Further it is found that Earth's temperature follows more closely decade variations in galactic cosmic ray flux and solar cycle length, than other solar activity parameters. The main conclusion is that the average state of the heliosphere affects Earth's climate.

Henrik Svensmark

1998-11-30T23:59:59.000Z

265

MCNP6 Cosmic-Source Option  

SciTech Connect

MCNP is a Monte Carlo radiation transport code that has been under development for over half a century. Over the last decade, the development team of a high-energy offshoot of MCNP, called MCNPX, has implemented several physics and algorithm improvements important for modeling galactic cosmic-ray (GCR) interactions with matter. In this presentation, we discuss the latest of these improvements, a new Cosmic-Source option, that has been implemented in MCNP6.

McKinney, Gregg W [Los Alamos National Laboratory; Armstrong, Hirotatsu [Los Alamos National Laboratory; James, Michael R [Los Alamos National Laboratory; Clem, John [University of Delaware, BRI; Goldhagen, Paul [DHS, National Urban Security Technology Laboratory

2012-06-19T23:59:59.000Z

266

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)  

ScienceCinema (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

2011-11-02T23:59:59.000Z

267

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)  

SciTech Connect

'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) [Director, Center for Energy Frontier Research in Extreme Environments; EFree Staff

2011-05-01T23:59:59.000Z

268

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

269

High intensity femtosecond enhancement cavities  

E-Print Network (OSTI)

To produce extreme ultraviolet radiation via high harmonic generation (HHG) in rare gases, light intensities in excess of 1014 W/cm 2 are required. Usually such high intensity are obtained by parametric amplification of ...

Abram, Gilberto

2009-01-01T23:59:59.000Z

270

High-energy cosmic neutrinos from spine-sheath BL Lac jets  

E-Print Network (OSTI)

We recently proposed that structured (spine-sheath) jets associated to BL Lac objects offer a suitable environment for the production of the extragalactic high-energy ($E>100$ TeV) neutrino recently revealed by IceCube. Our previous analysis was limited to low-power BL Lac objects. We extend our preliminary study to the entire BL Lac population. We assume that the power of cosmic rays as well as the radiative luminosity of the sheath depend linearly on the the jet power. In turn, we assume that the latter is well traced by the $\\gamma$-ray luminosity. We exploit the BL Lac $\\gamma$-ray luminosity function and its cosmic evolution as recently inferred from Fermi-LAT data to derive the expected neutrino cumulative intensity from the entire BL Lac population. When considering only the low-power BL Lacs, a large cosmic ray power for each source is required to account for the neutrino flux. Instead, if BL Lacs of all powers produce neutrinos, the power demand decreases, and the required cosmic ray power becomes of...

Tavecchio, F

2014-01-01T23:59:59.000Z

271

Development of Indian High Intensity Proton Accelerator  

E-Print Network (OSTI)

· Brinkman, Director, US-DOE-OS met with Dr. Banerjee and Dr. Grover several time #12;Status: MOU: Fermilab The Fermilab Tevatron has now passed on the energy frontier to LHC, following 25 years as the highest energy particle collider in the world. Fermilab operates the highest power long baseline neutrino

Quigg, Chris

272

A theory of Cosmic Rays  

E-Print Network (OSTI)

We present a theory of non-solar cosmic rays (CRs) based on a single type of CR source at all energies. The total luminosity of the Galaxy, the broken power-law spectra with their observed slopes, the position of the `knee(s)' and `ankle', and the CR composition and its variation with energy are all predicted in terms of very simple and completely `standard' physics. The source of CRs is extremely `economical': it has only one parameter to be fitted to the ensemble of all of the mentioned data. All other inputs are `priors', that is, theoretical or observational items of information independent of the properties of the source of CRs, and chosen to lie in their pre-established ranges. The theory is part of a `unified view of high-energy astrophysics' --based on the `Cannonball' model of the relativistic ejecta of accreting black holes and neutron stars. If correct, this model is only lacking a satisfactory theoretical understanding of the `cannon' that emits the cannonballs in catastrophic processes of accreti...

Dar, Arnon; Dar, Arnon; Rjula, Alvaro De

2008-01-01T23:59:59.000Z

273

A theory of Cosmic Rays  

E-Print Network (OSTI)

We present a theory of non-solar cosmic rays (CRs) in which the bulk of their observed flux is due to a single type of CR source at all energies. The total luminosity of the Galaxy, the broken power-law spectra with their observed slopes, the position of the `knee(s)' and `ankle', and the CR composition and its variation with energy are all predicted in terms of very simple and completely `standard' physics. The source of CRs is extremely `economical': it has only one parameter to be fitted to the ensemble of all of the mentioned data. All other inputs are `priors', that is, theoretical or observational items of information independent of the properties of the source of CRs, and chosen to lie in their pre-established ranges. The theory is part of a `unified view of high-energy astrophysics' --based on the `Cannonball' model of the relativistic ejecta of accreting black holes and neutron stars. The model has been extremely successful in predicting all the novel properties of Gamma Ray Bursts recently observed with help of the Swift satellite. If correct, this model is only lacking a satisfactory theoretical understanding of the `cannon' that emits the cannonballs in catastrophic processes of accretion.

Arnon Dar; Alvaro De Rujula

2006-06-19T23:59:59.000Z

274

Collection: High-Energy Cosmic Ray Event Data from the Pierre...  

Office of Scientific and Technical Information (OSTI)

High-Energy Cosmic Ray Event Data from the Pierre Auger Cosmic Ray Observatory Citation Details Title: High-Energy Cosmic Ray Event Data from the Pierre Auger Cosmic Ray...

275

Jupiter as a Giant Cosmic Ray Detector  

E-Print Network (OSTI)

We explore the feasibility of using the atmosphere of Jupiter to detect Ultra-High-Energy Cosmic Rays (UHECR's). The large surface area of Jupiter allows us to probe cosmic rays of higher energies than previously accessible. Cosmic ray extensive air showers in Jupiter's atmosphere could in principle be detected by the Large Area Telescope (LAT) on the Fermi observatory. In order to be observed, these air showers would need to be oriented toward the Earth, and would need to occur sufficiently high in the atmosphere that the gamma rays can penetrate. We demonstrate that, under these assumptions, Jupiter provides an effective cosmic ray "detector" area of $3.3 \\times 10^7$ km$^2$. We predict that Fermi-LAT should be able to detect events of energy $>10^{21}$ eV with fluence $10^{-7}$ erg cm$^{-2}$ at a rate of about one per month. The observed number of air showers may provide an indirect measure of the flux of cosmic rays $\\gtrsim 10^{20}$ eV. Extensive air showers also produce a synchrotron signature that may ...

Rimmer, Paul B; Helling, Christiane

2014-01-01T23:59:59.000Z

276

Cosmic rays and tests of fundamental principles  

E-Print Network (OSTI)

It is now widely acknowledged that cosmic rays experiments can test possible new physics directly generated at the Planck scale or at some other fundamental scale. By studying particle properties at energies far beyond the reach of any man-made accelerator, they can yield unique checks of basic principles. A well-known example is provided by possible tests of special relativity at the highest cosmic-ray energies. But other essential ingredients of standard theories can in principle be tested: quantum mechanics, uncertainty principle, energy and momentum conservation, effective space-time dimensions, hamiltonian and lagrangian formalisms, postulates of cosmology, vacuum dynamics and particle propagation, quark and gluon confinement, elementariness of particles... Standard particle physics or string-like patterns may have a composite origin able to manifest itself through specific cosmic-ray signatures. Ultra-high energy cosmic rays, but also cosmic rays at lower energies, are probes of both "conventional" and new Physics. Status, prospects, new ideas, and open questions in the field are discussed. The Post Scriptum shows that several basic features of modern cosmology naturally appear in a SU(2) spinorial description of space-time without any need for matter, relativity or standard gravitation. New possible effects related to the spinorial space-time structure can also be foreseen. Similarly, the existence of spin-1/2 particles can be naturally related to physics beyond Planck scale and to a possible pre-Big Bang era.

Luis Gonzalez-Mestres

2010-11-22T23:59:59.000Z

277

Managing Hardware Configurations and Data Products for the Canadian Hydrogen Intensity Mapping Experiment  

E-Print Network (OSTI)

The Canadian Hydrogen Intensity Mapping Experiment (CHIME) is an ambitious new radio telescope project for measuring cosmic expansion and investigating dark energy. Keeping good records of both physical configuration of its 1280 antennas and their analogue signal chains as well as the ~100 TB of data produced daily from its correlator will be essential to the success of CHIME. In these proceedings we describe the database-driven software we have developed to manage this complexity.

Hincks, Adam D

2014-01-01T23:59:59.000Z

278

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

279

Cosmic Ray Energy Measurement with EAS Cherenkov Light: Experiment QUEST and CORSIKA Simulation  

E-Print Network (OSTI)

A new method of a primary cosmic particle energy measurement with the extensive air shower (EAS) technique has been developed by exploiting: a) the joint analysis of the shower size, obtained by the EAS-TOP array, and of the EAS Cherenkov light lateral distribution (LDF), obtained by the QUEST array, and b) simulations based on the CORSIKA code. The method is based on the strict correlation between the size/energy ratio and the steepness of the Cherenkov light lateral distribution and has been compared with a "classical" one based on the Cherenkov light flux at a fixed distance (175 m) from the EAS core. The independence of the energy measurement both on the mass of primary particle and the hadronic interaction model used for the analysis is shown. Based on this approach the experimental integral intensity of cosmic rays flux with energy more than 3*10^15 eV is obtained with good systematic and statistical accuracy.

E. E. Korosteleva; L. A. Kuzmichev; V. V. Prosin; EAS-TOP COLLABORATION

2005-11-08T23:59:59.000Z

280

SOLAR ORIGIN OF CHANGES IN THE PRIMARY COSMIC RADIATION  

Science Journals Connector (OSTI)

SOLAR ORIGIN OF CHANGES IN THE PRIMARY COSMIC RADIATION...DEPARTMENT OF PHYSICS, UNIVERSITY OF CHICAGO SOLAR ORIGIN OF CHANGES IN THE PRIMARY COSMIC RADIATION...that any relationship of these variations to solar phenomena arose through in- direct processes...

J. A. Simpson

1957-01-01T23:59:59.000Z

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.


281

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...

Feng, Shaoyong

2011-10-21T23:59:59.000Z

282

Searching for Cosmic Accelerators via IceCube  

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

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,...

283

Spatial and temporal distribution of secondary cosmic-ray nucleon intensities and applications to  

E-Print Network (OSTI)

theoretical framework appropriate for cosmogenic dating. The most important parameter to be constrained and over the same altitudes. We attribute the difference to a combination of two factors: the neutron monitor is more sensitive to the higher end of the nucleon energy spectrum, and the shape of the nucleon

Zreda, Marek

284

A Common Solution of Two Cosmic Puzzles  

E-Print Network (OSTI)

The origin of the diffuse extragalactic gamma-ray background, which was measured with the large area telescope (LAT) aboard the Fermi satellite at energy below 820 GeV, and of the diffuse cosmic background of neutrinos, which was observed at much higher energies with the IceCube detector deep under the south pole ice, are among the current unsolved major cosmic puzzles. Here we show that their properties indicate a common origin: the decay of mesons produced in collisions of cosmic rays accelerated in relativistic jets with matter in/near source. Moreover, their properties are those expected if their common source is the highly relativistic jets that produce the long duration gamma ray bursts in core collapse supernovae of type Ic, which take place mostly in the densest regions of giant molecular clouds in star forming galaxies.

Dado, Shlomo

2014-01-01T23:59:59.000Z

285

The Spine of the Cosmic Web  

Science Journals Connector (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. Aragn-Calvo; Erwin Platen; Rien van de Weygaert; Alexander S. Szalay

2010-01-01T23:59:59.000Z

286

Anomalous isotopic composition of cosmic rays  

SciTech Connect

Recent measurements of nonsolar isotopic patterns for the elements neon and (perhaps) magnesium in cosmic rays are interpreted within current models of stellar nucleosynthesis. One possible explanation is that the stars currently responsible for cosmic-ray synthesis in the Galaxy are typically super-metal-rich by a factor of two to three. Other possibilities include the selective acceleration of certain zones or masses of supernovas or the enhancement of /sup 22/Ne in the interstellar medium by mass loss from red giant stars and planetary nebulas. Measurements of critical isotopic ratios are suggested to aid in distinguishing among the various possibilities. Some of these explanations place significant constraints on the fraction of cosmic ray nuclei that must be fresh supernova debris and the masses of the supernovas involved. 1 figure, 3 tables.

Woosley, S.E.; Weaver, T.A.

1980-06-20T23:59:59.000Z

287

Weyl's principle, cosmic time and quantum fundamentalism  

E-Print Network (OSTI)

We examine the necessary physical underpinnings for setting up the cosmological standard model with a global cosmic time parameter. In particular, we discuss the role of Weyl's principle which asserts that cosmic matter moves according to certain regularity requirements. After a brief historical introduction to Weyl's principle we argue that although the principle is often not explicitly mentioned in modern standard texts on cosmology, it is implicitly assumed and is, in fact, necessary for a physically well-defined notion of cosmic time. We finally point out that Weyl's principle might be in conflict with the wide-spread idea that the universe at some very early stage can be described exclusively in terms of quantum theory.

Svend E. Rugh; Henrik Zinkernagel

2010-06-30T23:59:59.000Z

288

Weyl's principle, cosmic time and quantum fundamentalism  

E-Print Network (OSTI)

We examine the necessary physical underpinnings for setting up the cosmological standard model with a global cosmic time parameter. In particular, we discuss the role of Weyl's principle which asserts that cosmic matter moves according to certain regularity requirements. After a brief historical introduction to Weyl's principle we argue that although the principle is often not explicitly mentioned in modern standard texts on cosmology, it is implicitly assumed and is, in fact, necessary for a physically well-defined notion of cosmic time. We finally point out that Weyl's principle might be in conflict with the wide-spread idea that the universe at some very early stage can be described exclusively in terms of quantum theory.

Rugh, Svend E

2010-01-01T23:59:59.000Z

289

Cosmic string structure at the gravitational radiation scale  

Science Journals Connector (OSTI)

We use our model of the small scale structure on cosmic strings to develop further the result of Siemens, Olum, and Vilenkin that the gravitational radiation length scale on cosmic strings is smaller than the previously assumed ?G?t. We discuss some of the properties of cosmic string loops at this cutoff scale, and we argue that recent network simulations point to two populations of cosmic string loops, one near the horizon scale and one near the gravitational radiation cutoff.

Joseph Polchinski and Jorge V. Rocha

2007-06-07T23:59:59.000Z

290

The current status of observational constraints on cosmic strings  

SciTech Connect

The observational restrictions on the cosmic string scenario for the formation of large scale structure are evaluated. this restrictions are due to the spectrum of gravitational radiation emitted by oscillating string loops, anisotropies in the cosmic microwave background caused by the strings, and evaporating black holes formed from collapsed cosmic string loops. It is shown that the only free parameter of the scenario, the cosmic string mass-per-unit-length, {mu}, is severely restricted.

Caldwell, R.R.

1993-10-01T23:59:59.000Z

291

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)

292

A New View of the Cosmic Landscape  

E-Print Network (OSTI)

In this scenario, a generic meta-stable deSitter vacuum site in the cosmic landscape in string theory has a very short lifetime. Typically, the smaller is the vacuum energy of a meta-stable site, the longer is its lifetime. This view of the landscape can provide a qualitative dynamical explanation why the dark energy of our universe is so small. The argument for this scenario is based on resonance tunneling, a well-known quantum mechanical phenomenon, the topography of the landscape, and the vastness of the cosmic landscape. Mapping the topography of the landscape, even if only in a small region, will test the validity of this scenario.

S. -H. Henry Tye

2007-04-16T23:59:59.000Z

293

On horizons and the cosmic landscape  

E-Print Network (OSTI)

Susskind claims in his recent book The Cosmic Landscape that evidence for the existence and nature of `pocket universes' in a multiverse would be available in the detailed nature of the Cosmic Blackbody Background Radiation that constantly bathes all parts of our observable universe. I point out that acceptance of the complex chain of argument involved does not imply possible experimental verification of multiverses at the present time. Rather this claim relates only to theoretically possible observations in the very far future of the universe.

George F R Ellis

2006-03-15T23:59:59.000Z

294

SHIELDING ASTRONAUTS FROM COSMIC RAYS E. N. Parker  

E-Print Network (OSTI)

enshrouded mass of Earth is subject to a continuing low dose rate of galactic cosmic radiation. Exposure years. The best available estimates of the accumulated cosmic radiation damage to the astronauts predict of the ongoing radiation damage by the cosmic rays. Unfortunately there is very little information available

Shepherd, Simon

295

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

296

Galaxy properties and the cosmic web in simulations  

Science Journals Connector (OSTI)

......Article Galaxy properties and the cosmic web in simulations Ofer Metuki 1 Noam I. Libeskind...simulations within the framework of the cosmic web as formulated by Hoffman et-al., focusing...knots - the four elements of the cosmic web. We find that the mass functions of haloes......

Ofer Metuki; Noam I. Libeskind; Yehuda Hoffman; Robert A. Crain; Tom Theuns

2015-01-01T23:59:59.000Z

297

Benchmarking local public libraries using non-parametric frontier methods: A case study of Flanders  

Science Journals Connector (OSTI)

Abstract Being faced with significant budget cuts and continual pressure to do more with less, issues of efficiency and effectiveness became a priority for local governments in most countries. In this context, benchmarking is widely acknowledged as a powerful tool for local performance management and for improving the efficiency and effectiveness of local service delivery. Performance benchmarking exercises are regularly carried out using ratio analysis, by comparing single indicators. Since this approach offers only limited assessments in absolute terms, it is difficult for decision-makers to track and improve overall performance. Therefore, the use of non-parametric frontier methods, namely free disposal hull (FDH) and data envelopment analysis (DEA) is presented as an alternative technique for benchmarking the performance of organizations in relative terms. The potential applications and strengths of these non-parametric frontier methods for benchmarking the efficiency of local public services are highlighted by applying FDH and DEA techniques to the local public libraries in Flanders. Incorporating all possible paths of expansion both in space and in time enables a focus on sustainability within efficiency benchmarking.

Jesse Stroobants; Geert Bouckaert

2014-01-01T23:59:59.000Z

298

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

299

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.

300

Frontiers in Offshore Geotechnics: ISFOG 2005 Gourvenec & Cassidy (eds) 2005 Taylor & Francis Group, London, ISBN 0 415 39063 X  

E-Print Network (OSTI)

Frontiers in Offshore Geotechnics: ISFOG 2005 ­ Gourvenec & Cassidy (eds) © 2005 Taylor & Francis research work on the design of suction caisson foundations for offshore wind turbines. Most of the relevant as anchors, principally in clays, and have also been used as foundations for a small number of offshore

Byrne, Byron

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

Frontiers in Laser Cooling, Single-Molecule Biophysics, and Enrgy Science: A Talk from Leo Holberg and Allen Mills  

ScienceCinema (OSTI)

Leo Holberg and Allen Mills present a talk at Frontiers in Laser Cooling, Single-Molecule Biophysics and Energy Science, a scientific symposium honoring Steve Chu, director of Lawrence Berkeley National Laboratory and recipient of the 1997 Nobel Prize in Physics. The symposium was held August 30, 2008 in Berkeley.

Holberg, Leo; Mills, Allen [NIST

2011-04-28T23:59:59.000Z

302

Frontiers in Offshore Geotechnics: ISFOG 2005 Gourvenec & Cassidy (eds) 2005 Taylor & Francis Group, London, ISBN 0 415 39063 X  

E-Print Network (OSTI)

considered as founda- tions for offshore wind turbines (Byrne & Houlsby 2003). The wind turbine structures, but the main differences in loads on the foundations for offshore wind turbines as compared to typical oilFrontiers in Offshore Geotechnics: ISFOG 2005 ­ Gourvenec & Cassidy (eds) © 2005 Taylor & Francis

Byrne, Byron

303

Capturing frontier research in grant proposals and initial analysis of the comparison between model vs. peer review1  

E-Print Network (OSTI)

vs. peer review1 Dirk Holste* , Thomas Scherngell* , Ivana Roche**, Marianne Hörlesberger-statistical model for inferring attributes of ,,frontier research in peer-reviewed research proposals submitted of a proposal to be accepted and compares outcomes between the model and peer-review decision, with the goal

Paris-Sud XI, Université de

304

Energy spectrum of cosmic-ray muons  

Science Journals Connector (OSTI)

The energy spectrum of cosmic-ray muons at sea-level is calculated by the ... in good agreement with the observed data of muons with the zenith angles of 0 and ... the scaling model is valid up to the muon energy

H. Komori; K. Mitsui

305

Accelerator Data for Cosmic Ray Physics  

E-Print Network (OSTI)

I present selected examples of accelerator data, mainly from hadron colliders, that are relevant for understanding cosmic ray showers. I focus on the forward region, $x_{Feynman} > 0.05$, where high energy data are scarce, since the emphasis in collider physics became high-$p_T$ phenomena.

M. G. Albrow

2010-09-21T23:59:59.000Z

306

Catching the highest energy cosmic rays  

Science Journals Connector (OSTI)

......interest in very-high-energy cosmic rays, which I define arbitrarily as those of energies above 3 1018 eV, the devices...Pierre Auger Observatory in Argentina - and what has been deduced...the measurements of the energy spectrum and arrival directions......

Alan A Watson

2009-04-01T23:59:59.000Z

307

Student Projects in Cosmic Ray Detection  

Science Journals Connector (OSTI)

The Alberta Large?area Time?coincidence Array (ALTA) study has been in existence for about 10 years under the direction of Jim Pinfold of the Centre for Particle Physics at the University of Alberta.1 The purpose of the ALTA project is to involve Alberta high schools and primarily their physics classes to assist in the detection of the presence of cosmic ray bursts in different Alberta locations. These cosmic rays involve highspeed elementary particles many from far outside our solar system and even from outside our galaxy. These particles collide with the particles in our atmosphere break up these molecules into rather exotic elementary particles which often reach the surface of the Earth and can be detected by fairly simple equipment. One of the objectives of ALTA is to determine the nature of some of the most energetic cosmic ray particles whose origin is still not known. Recently 2the Pierre Auger Collaboration has confirmed that the highest energy cosmic rays appear to be coming from nearby galaxies. The mechanism for their production is still not well understood.

W. Brouwer; J. Pinfold; R. Soluk; B. McDonough; V. Pasek; Zheng Bao?shan

2009-01-01T23:59:59.000Z

308

Cosmic IR Backgrounds Ned Wright (UCLA)  

E-Print Network (OSTI)

Cosmic IR Backgrounds by Ned Wright (UCLA) http://www.astro.ucla.edu/~wright/intro.html See: · http://www.astro.ucla.edu/~wright/cosmolog.htm · http://www.astro.ucla.edu/~wright/DIRBE · http://www.astro.ucla.edu/~wright/CIBR · http

Wright, Edward L. "Ned"

309

Supernova Remnants, Cosmic Rays, and GLAST  

SciTech Connect

The shock waves of supernova remnants (SNRs) are the traditional sources of Galactic cosmic rays, at least up to about 3000 TeV (the 'knee' energy in the cosmic-ray spectrum). In the last decade or so, X-ray observations have confirmed in a few SNRs the presence of synchrotron-X-ray-emitting electrons with energies of order 100 TeV. TeV photons from SNRs have been observed with ground-based air Cerenkov telescopes as well, but it is still unclear whether they are due to hadronic processes (inelastic p-p scattering of cosmic-ray protons from thermal gas, with secondary neutral pions decaying to gamma rays), or to leptonic processes (inverse-Compton upscattering of cosmic microwave background photons, or bremsstrahlung). The spatial structure of synchrotron X-rays as observed with the Chandra X-ray Observatory suggests the remarkable possibility that magnetic fields are amplified by orders of magnitude in strong shock waves. The electron spectra inferred from X-rays reach 100 TeV, but at that energy are cutting off steeply, well below the 'knee' energy. Are the cutoff processes due only to radiative losses so that ion spectra might continue unsteepened? Can we confirm the presence of energetic ions in SNRs at all? Are typical SNRs capable of supplying the pool of Galactic cosmic rays? Is strong magnetic-field amplification a property of strong astrophysical shocks in general? These major questions require the next generation of observational tools. I shall outline the theoretical and observational framework of particle acceleration to high energies in SNRs, and shall describe how GLAST will advance this field.

Reynolds, Steve (North Carolina State University) [North Carolina State University

2006-02-13T23:59:59.000Z

310

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

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

teChnologIes Program IntroduCtIon the research and development (r&d) portfolio for energy-Intensive Processes (eIP) addresses the top technology opportunities to save energy...

311

Consequences of the common origin of the knee and ankle in Cosmic Ray Physics  

E-Print Network (OSTI)

The differential energy spectrum of the cosmic radiation from solar modulation energies up to 5x10**19 eV is correctly predicted by a recent theory of the knee and ankle which uses only one normalization point. This remarkable quantitative result, spanning over many decades in energy and intensity, along with the existence of the second knee at 6x10**17 eV, is obtained assuming constant spectral indices of individual ions at the cosmic-ray sources and no other critical hypotheses. In this study the chemical composition of the cosmic radiation is evaluated as a direct consequence of the theory. The computed mean logarithmic mass exhibits a rising trend from 1.8 to 3.0 in the range 10**15-10**17 eV, a maximum value of 3.2 at 3x10**17 eV, and a characteristic lightening above 3x10**17 eV up to 4x10**18 eV. All of these distinctive features are in accord with the data of many experiments. Two additional consequences intrinsic to the theory are qualitatively discussed: (1) some limitative bounds on the mechanism a...

Codino, Antonio

2009-01-01T23:59:59.000Z

312

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

313

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)

314

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

315

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

316

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

317

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.

Thacker, Louis H. (Knoxville, TN)

1995-01-01T23:59:59.000Z

318

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.

Thacker, Louis H. (Knoxville, TN)

1994-01-01T23:59:59.000Z

319

"The Most Hazardous and Dangerous and Greatest Adventure on Which Man Has Ever Embarked": The Frontier in Presidential Pro-Space Discourse, 1957-1963  

E-Print Network (OSTI)

Since the inception of the US Space Program, space exploration has been linked in public discourse to the cluster of ideas and images constituting "the frontier." In the seven years between 1957 and 1963, Presidents ...

Leyerzapf, Amy Beth

2011-12-31T23:59:59.000Z

320

Angular correlation of cosmic neutrinos with ultrahigh-energy cosmic rays and implications for their sources  

E-Print Network (OSTI)

Cosmic neutrino events detected by the IceCube Neutrino Observatory with energy $\\gtrsim 30$ TeV have poor angular resolutions to reveal their origin. Ultrahigh-energy cosmic rays (UHECRs), with better angular resolutions at $>60$ EeV energies, can be used to check if the same astrophysical sources are responsible for producing both neutrinos and UHECRs. We test this hypothesis, with statistical methods which emphasize invariant quantities, by using data from the Pierre Auger Observatory, Telescope Array and past cosmic-ray experiments. We find that the arrival directions of the cosmic neutrinos are correlated with $\\ge 100$ EeV UHECR arrival directions at confidence level $\\approx 93\\%$. The strength of the correlation decreases with decreasing UHECR energy and no correlation exists at energy $\\sim 60$ EeV. A search in astrophysical databases within $3^\\circ$ of the arrival directions of UHECRs with energy $\\ge 100$ EeV, that are correlated with the IceCube cosmic neutrinos, resulted in 18 sources from the S...

Moharana, Reetanjali

2015-01-01T23:59:59.000Z

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.


321

THE MODULATION OF GALACTIC COSMIC-RAY ELECTRONS IN THE HELIOSHEATH  

SciTech Connect

Voyager 1 has observed strong increases in the intensities of 2-160 MeV electrons since crossing the termination shock of the heliosphere in 2004 December. Before this time these intensities were submerged below the detector background, except for occasional transient events. These increases are large compared to the concurrent increases of positive ions such as H, He, and O. A significant part is probably due to temporal effects as the heliosphere was recovering to solar minimum conditions from 2005 to early 2010. The intensity observed by Voyager 2 since its crossing of the shock in 2007 September is 5-10 times lower than that observed by Voyager 1, which is so low that the electron intensity may still be below the background produced by high-energy protons in the detector. This points to a large north-south asymmetry in the properties of the heliosheath. It is shown that the observations suggest that these electrons are not freshly accelerated on the termination shock, but rather that they are of galactic origin-while they may be re-accelerated by that shock. In this paper, these intensities are modeled with numerical solutions of the cosmic-ray transport equation. It is shown that because they are relativistic, the electrons are much more sensitive to the form of the diffusion coefficient at low rigidities than ions, and that this can explain the asymmetry.

Caballero-Lopez, R. A. [Instituto de Geofisica, UNAM, 04510 Mexico, D. F. (Mexico); Moraal, H. [Unit for Space Physics, School of Physical and Chemical Sciences, North-West University, Potchefstroom 2520 (South Africa); McDonald, F. B., E-mail: rogelioc@geofisica.unam.m [Institute for Physical Science and Technology, University of Maryland, College Park, MD 20742 (United States)

2010-12-10T23:59:59.000Z

322

The Cosmic Evolution Survey (COSMOS) -- Overview  

E-Print Network (OSTI)

The Cosmic Evolution Survey (COSMOS) is designed to probe the correlated evolution of galaxies, star formation, active galactic nuclei (AGN) and dark matter (DM) with large-scale structure (LSS) over the redshift range z $> 0.5 $ to 6. The survey includes multi-wavelength imaging and spectroscopy from X-ray to radio wavelengths covering a 2 $\\sq$\\deg area, including HST imaging. Given the very high sensitivity and resolution of these datasets, COSMOS also provides unprecedented samples of objects at high redshift with greatly reduced cosmic variance, compared to earlier surveys. Here we provide a brief overview of the survey strategy, the characteristics of the major COSMOS datasets, and summarize the science goals.

Scoville, N Z; Brusa, M; Capak, P; Carollo, C M; Elvis, M; Giavalisco, M; Guzzo, L; Hasinger, G; Impey, C; Kneib, J P; LeFevre, O; Lilly, S J; Mobasher, B; Renzini, A; Rich, R M; Sanders, D B; Schinnerer, E; Schminovich, D; Shopbell, P; Taniguchi, Y; Tyson, N D

2006-01-01T23:59:59.000Z

323

The Cosmic Evolution Survey (COSMOS) -- Overview  

E-Print Network (OSTI)

The Cosmic Evolution Survey (COSMOS) is designed to probe the correlated evolution of galaxies, star formation, active galactic nuclei (AGN) and dark matter (DM) with large-scale structure (LSS) over the redshift range z $> 0.5 $ to 6. The survey includes multi-wavelength imaging and spectroscopy from X-ray to radio wavelengths covering a 2 $\\sq$\\deg area, including HST imaging. Given the very high sensitivity and resolution of these datasets, COSMOS also provides unprecedented samples of objects at high redshift with greatly reduced cosmic variance, compared to earlier surveys. Here we provide a brief overview of the survey strategy, the characteristics of the major COSMOS datasets, and summarize the science goals.

N. Scoville; H. Aussel; M. Brusa; P. Capak; C. M. Carollo; M. Elvis; M. Giavalisco; L. Guzzo; G. Hasinger; C. Impey; J. -P. Kneib; O. LeFevre; S. J. Lilly; B. Mobasher; A. Renzini; R. M. Rich; D. B. Sanders; E. Schinnerer; D. Schminovich; P. Shopbell; Y. Taniguchi; N. D. Tyson

2006-12-12T23:59:59.000Z

324

The Cosmic Evolution Survey (COSMOS): Overview  

Science Journals Connector (OSTI)

The Cosmic Evolution Survey (COSMOS) is designed to probe the correlated evolution of galaxies, star formation, active galactic nuclei (AGNs), and dark matter (DM) with large-scale structure (LSS) over the redshift range z > 0.5-6. The survey includes multiwavelength imaging and spectroscopy from X-ray-to-radio wavelengths covering a 2 deg2 area, including HST imaging. Given the very high sensitivity and resolution of these data sets, COSMOS also provides unprecedented samples of objects at high redshift with greatly reduced cosmic variance, compared to earlier surveys. Here we provide a brief overview of the survey strategy, the characteristics of the major COSMOS data sets, and a summary the science goals.

N. Scoville; H. Aussel; M. Brusa; P. Capak; C. M. Carollo; M. Elvis; M. Giavalisco; L. Guzzo; G. Hasinger; C. Impey; J.-P. Kneib; O. LeFevre; S. J. Lilly; B. Mobasher; A. Renzini; R. M. Rich; D. B. Sanders; E. Schinnerer; D. Schminovich; P. Shopbell; Y. Taniguchi; N. D. Tyson

2007-01-01T23:59:59.000Z

325

Can Cosmic Structure form without Dark Matter?  

SciTech Connect

One of the prime pieces of evidence for dark matter is the observation of large overdense regions in the universe. Since we know from the cosmic microwave background that the regions that contained the most baryons when the universe was {approx} 400, 000 years old were overdense by only one part in ten thousand, perturbations had to have grown since then by a factor greater than (1 + z{sub *}) {approx_equal} 1180 where z{sub *} is the epoch of recombination. This enhanced growth does not happen in general relativity, so dark matter is needed in the standard theory. We show here that enhanced growth can occur in alternatives to general relativity, in particular in Bekenstein's relativistic version of Modified Newtonian Dynamics (MOND). The vector field introduced in that theory for a completely different reason plays a key role in generating the instability that produces large cosmic structures today.

Dodelson, Scott; /Fermilab /Chicago U., Astron. Astrophys. Ctr.; Liguori, Michele; /Fermilab /Padua U. /INFN, Padua

2006-08-01T23:59:59.000Z

326

Can Cosmic Structure form without Dark Matter?  

E-Print Network (OSTI)

One of the prime pieces of evidence for dark matter is the observation of large overdense regions in the universe. Since we know from the cosmic microwave background that the regions that contained the most baryons when the universe was ~400,000 years old were overdense by only one part in ten thousand, perturbations had to have grown since then by a factor greater than $(1+z_*)\\simeq 1180$ where $z_*$ is the epoch of recombination. This enhanced growth does not happen in general relativity, so dark matter is needed in the standard theory. We show here that enhanced growth can occur in alternatives to general relativity, in particular in Bekenstein's relativistic version of MOdified Newtonian Dynamics (MOND). The vector field introduced in that theory for a completely different reason plays a key role in generating the instability that produces large cosmic structures today.

Scott Dodelson; Michele Liguori

2006-08-29T23:59:59.000Z

327

Wiggly cosmic strings accrete dark energy  

E-Print Network (OSTI)

This paper deals with a study of the cylindrically symmetric accretion of dark energy with equation of state $p=w\\rho$ onto wiggly straight cosmic strings. We have obtained that when $w>-1$ the linear energy density in the string core gradually increases tending to a finite maximum value as time increases for all considered dark energy models. On the regime where the dominant energy condition is violated all such models predict a steady decreasing of the linear energy density of the cosmic strings as phantom energy is being accreted. The final state of the string after such an accretion process is a wiggleless defect. It is argued however that if accreation of phantom energy would proceed by successive quantum steps then the defect would continue losing linear energy density until a minimum nonzero value which can be quite smaller than that corresponding to the unperturbed string.

Pedro F. Gonzalez-Diaz; Jose A. Jimenez Madrid

2005-06-29T23:59:59.000Z

328

The Pierre Auger Cosmic Ray Observatory  

E-Print Network (OSTI)

The Pierre Auger Observatory, located on a vast, high plain in western Argentina, is the world's largest cosmic ray observatory. The objectives of the Observatory are to probe the origin and characteristics of cosmic rays above $10^{17}$ eV and to study the interactions of these, the most energetic particles observed in nature. The Auger design features an array of 1660 water-Cherenkov particle detector stations spread over 3000 km$^2$ overlooked by 24 air fluorescence telescopes. In addition, three high elevation fluorescence telescopes overlook a 23.5 km$^2$, 61 detector infill array. The Observatory has been in successful operation since completion in 2008 and has recorded data from an exposure exceeding 40,000 km$^2$ sr yr. This paper describes the design and performance of the detectors, related subsystems and infrastructure that make up the Auger Observatory.

,

2015-01-01T23:59:59.000Z

329

The Cosmic Microwave Background and Particle Physics  

E-Print Network (OSTI)

In forthcoming years, connections between cosmology and particle physics will be made increasingly important with the advent of a new generation of cosmic microwave background (CMB) experiments. Here, we review a number of these links. Our primary focus is on new CMB tests of inflation. We explain how the inflationary predictions for the geometry of the Universe and primordial density perturbations will be tested by CMB temperature fluctuations, and how the gravitational waves predicted by inflation can be pursued with the CMB polarization. The CMB signatures of topological defects and primordial magnetic fields from cosmological phase transitions are also discussed. Furthermore, we review current and future CMB constraints on various types of dark matter (e.g. massive neutrinos, weakly interacting massive particles, axions, vacuum energy), decaying particles, the baryon asymmetry of the Universe, ultra-high-energy cosmic rays, exotic cosmological topologies, and other new physics.

Marc Kamionkowski; Arthur Kosowsky

1999-04-09T23:59:59.000Z

330

Diffusion coefficient and radial gradient of galactic cosmic rays  

E-Print Network (OSTI)

We present the temporal changes of the diffusion coefficient K of galactic cosmic rays (GCRs) at the Earth orbit calculated based on the experimental data using two different methods. The first approach is based on the Parker convection-diffusion approximation of GCR modulation [1]: i.e. K~Vr=dI where dI is the variation of the GCR intensity measured by neutron monitors (NM),V is the solar wind velocity and r is the radial distance. The second approach is based on the interplanetary magnetic field (IMF) data. It was suggested that parallel mean free path can be expressed in terms of B as in [2]-[4]. Using data of the product of the parallel mean free path and radial gradient of GCR calculated based on the GCR anisotropy data (Ahluwalia et al., this conference ICRC 2013, poster ID: 487 [5]), we estimate the temporal changes of the radial gradient of GCR at the Earth orbit. We show that the radial gradient exhibits a strong solar cycle dependence (11-year variation) and a weak solar magnetic cycle dependence (2...

Modzelewska, Renata

2015-01-01T23:59:59.000Z

331

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

332

The Penumbra at Geomagnetic Latitude 20 and the Energy Spectrum of Primary Cosmic Radiation  

Science Journals Connector (OSTI)

The method of obtaining the penumbra presented in a previous paper is applied to the following energies: r=0.385,0.400,0.425,0.450and0.500 Strmer at a geomagnetic latitude of 20. Two graphs showing the variation of the penumbra with the energy are derived from the (?1,?) diagrams of these energies: one at a constant zenith angle of 60, and the other along the east-west plane. If the number of primaries is assumed to vary inversely as the 2.8 power of their energy, the contribution of the penumbra to the directional intensity at a zenith angle of 60 is calculated, and is shown to be far from negligible. The calculated intensities are quite sensitive to the energy distribution used, and this suggests a possible method for determining the energy spectrum of primary cosmic rays.

R. Albagli Hutner

1939-04-01T23:59:59.000Z

333

Polarization of the Atmosphere as a Foreground for Cosmic Microwave Background Polarization Experiments  

E-Print Network (OSTI)

We quantify the level of polarization of the atmosphere due to Zeeman splitting of oxygen in the Earth's magnetic field and compare it to the level of polarization expected from the polarization of the cosmic microwave background radiation. The analysis focuses on the effect at mid-latitudes and at large angular scales. We find that from stratospheric balloon borne platforms and for observations near 100 GHz the atmospheric linear and circular polarized intensities is about 10^{-12} and 100 x 10^{-9} K, respectively, making the atmosphere a negligible source of foreground. From the ground the linear and circular polarized intensities are about 10^{-9} and 100 x 10^{-6} K, making the atmosphere a potential source of foreground for the CMB E (B) mode signal if there is even a 1% (0.01%) conversion of circular to linear polarization in the instrument.

Shaul Hanany; Philip Rosenkranz

2003-07-02T23:59:59.000Z

334

Scaling Solution for Small Cosmic String Loops  

Science Journals Connector (OSTI)

The equation governing the time evolution of the number density of loops in a cosmic string network is a detailed balance determined by energy conservation. We solve this equation with the inclusion of the gravitational radiation effect, which causes the loops to shrink (and eventually decay) as time elapses. The solution approaches a scaling regime in which the total energy density in loops remains finite, converging both in the infrared and in the ultraviolet.

Jorge V. Rocha

2008-02-21T23:59:59.000Z

335

Cosmic string loops, large and small  

Science Journals Connector (OSTI)

We extend our earlier model of the small-scale structure of cosmic string networks through an improved treatment of the separation of long and short scales. We find that the production of small loops (at the gravitational radiation scale) is a robust feature of string networks, in addition to a population of loops near the horizon scale. We obtain quantitative agreement with the scaling of loop production functions as found in simulations by two groups.

Florian Dubath; Joseph Polchinski; Jorge V. Rocha

2008-06-23T23:59:59.000Z

336

Cosmic Microwave Background: Past, Future, and Present  

E-Print Network (OSTI)

I explain the origin and evolution of anisotropies in the Cosmic Microwave Background (CMB) and argue that upcoming experiments will measure cosmological and fundamental parameters very accurately. Most of the paper focuses on present data, which strongly suggest that the universe is flat. Several arguments are given to prove that present data sets are not contaminated by systematics. New techniques to compare different experiments visually are introduced. These are illustrated for two years of the MSAM and Python experiments.

Scott Dodelson

1999-12-22T23:59:59.000Z

337

Phenomenology of cosmic ray air showers  

E-Print Network (OSTI)

The properties of cosmic rays with energies above 1PeV have to be deduced from the spacetime structure and particle content of the air showers which they initiate. In this review, a summary of the phenomenology of these giant air showers is presented. We describe the hadronic interaction models used to extrapolate results from collider data to ultra high energies, an also the main electromagnetic processes that govern the longitudinal shower evolution as well as the lateral spread of particles.

M. T. Dova

2005-05-30T23:59:59.000Z

338

Cosmic Rays around $10^{18} $eV: Implications of Contemporary Measurements on the Origin of the Ankle Feature  

E-Print Network (OSTI)

The impressive power-law decay of the energy spectrum of cosmic rays over more than thirty orders of magnitude in intensity and for energies ranging over eleven decades between $\\simeq 10^9 $eV and $\\simeq 10^{20} $eV is actually dotted with small irregularities. These irregularities are highly valuable for uncovering and understanding the modes of production and propagation of cosmic rays. They manifest themselves through changes in the spectral index characterising the observed power laws. One of these irregularities, known as the \\textit{ankle}, is subject to conflicting interpretations for many years. If contemporary observations characterising it have shed new lights, they are still far from being able to deliver all the story. The purpose of this contribution is to give an overview of the physics of cosmic rays in the energy range where the transition between Galactic and extragalactic cosmic rays is expected to occur, and to deliver several lines of thought about the origin of the ankle.

Deligny, Olivier

2014-01-01T23:59:59.000Z

339

Suzaku Observation of the Fermi Cygnus Cocoon: Search for a Signature of Young Cosmic-Ray Electrons  

E-Print Network (OSTI)

The origin of Galactic cosmic rays remains unconfirmed, but promising candidates for their sources are found in star-forming regions. We report a series of X-ray observations, with Suzaku, toward the nearby star-forming region of Cygnus X. They aim at comparing diffuse X-ray emissions on and off the $\\gamma$-ray cocoon of hard cosmic rays revealed by Fermi LAT. After excluding point sources and small-scale structures and subtracting the non-X-ray and cosmic X-ray backgrounds, the 2--10~keV X-ray intensity distribution is found to monotonically decrease with increasing Galactic latitude. This indicates that most of the extended emission detected by Suzaku originates from the Galactic ridge. In two observations, we derive upper limits of $3.4 \\times 10^{-8}~{\\rm erg~s^{-1}~cm^{-2}~sr^{-1}}$ and $1.3 \\times 10^{-8}~{\\rm erg~s^{-1}~cm^{-2}~sr^{-1}}$ to X-ray emission in the 2--10 keV range from the gamma-ray cocoon. These limits exclude the presence of cosmic-ray electrons with energies above about 50 TeV at a fl...

Mizuno, T; Takahashi, H; Hayashi, K; Yamazaki, R; Grenier, I; Tibaldo, L

2015-01-01T23:59:59.000Z

340

Statistics and geometry of cosmic voids  

SciTech Connect

We introduce new statistical methods for the study of cosmic voids, focusing on the statistics of largest size voids. We distinguish three different types of distributions of voids, namely, Poisson-like, lognormal-like and Pareto-like distributions. The last two distributions are connected with two types of fractal geometry of the matter distribution. Scaling voids with Pareto distribution appear in fractal distributions with box-counting dimension smaller than three (its maximum value), whereas the lognormal void distribution corresponds to multifractals with box-counting dimension equal to three. Moreover, voids of the former type persist in the continuum limit, namely, as the number density of observable objects grows, giving rise to lacunar fractals, whereas voids of the latter type disappear in the continuum limit, giving rise to non-lacunar (multi)fractals. We propose both lacunar and non-lacunar multifractal models of the cosmic web structure of the Universe. A non-lacunar multifractal model is supported by current galaxy surveys as well as cosmological N-body simulations. This model suggests, in particular, that small dark matter halos and, arguably, faint galaxies are present in cosmic voids.

Gaite, Jos, E-mail: jose.gaite@upm.es [Instituto de Microgravedad IDR, ETS Ingenieros Aeronuticos, Universidad Politcnica de Madrid, E-28040 Madrid (Spain)

2009-11-01T23:59:59.000Z

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.


341

Dark energy perturbations and cosmic coincidence  

E-Print Network (OSTI)

While there is plentiful evidence in all fronts of experimental cosmology for the existence of a non-vanishing dark energy (DE) density \\rho_D in the Universe, we are still far away from having a fundamental understanding of its ultimate nature and of its current value, not even of the puzzling fact that \\rho_D is so close to the matter energy density \\rho_M at the present time (i.e. the so-called "cosmic coincidence" problem). The resolution of some of these cosmic conundrums suggests that the DE must have some (mild) dynamical behavior at the present time. In this paper, we examine some general properties of the simultaneous set of matter and DE perturbations (\\delta\\rho_M, \\delta\\rho_D) for a multicomponent DE fluid. Next we put these properties to the test within the context of a non-trivial model of dynamical DE (the LXCDM model) which has been previously studied in the literature. By requiring that the coupled system of perturbation equations for \\delta\\rho_M and \\delta\\rho_D has a smooth solution throughout the entire cosmological evolution, that the matter power spectrum is consistent with the data on structure formation and that the "coincidence ratio" r=\\rho_D/\\rho_M stays bounded and not unnaturally high, we are able to determine a well-defined region of the parameter space where the model can solve the cosmic coincidence problem in full compatibility with all known cosmological data.

Javier Grande; Ana Pelinson; Joan Sola

2009-04-29T23:59:59.000Z

342

Solar panels as cosmic-ray detectors  

E-Print Network (OSTI)

Due to fundamental limitations of accelerators, only cosmic rays can give access to centre-of- mass energies more than one order of magnitude above those reached at the LHC. In fact, extreme energy cosmic rays (1018 eV - 1020 eV) are the only possibility to explore the 100 TeV energy scale in the years to come. This leap by one order of magnitude gives a unique way to open new horizons: new families of particles, new physics scales, in-depth investigations of the Lorentz symmetries. However, the flux of cosmic rays decreases rapidly, being less than one particle per square kilometer per year above 1019 eV: one needs to sample large surfaces. A way to develop large-effective area, low cost, detectors, is to build a solar panel-based device which can be used in parallel for power generation and Cherenkov light detection. Using solar panels for Cherenkov light detection would combine power generation and a non-standard detection device.

Stella, Carlo; Assis, Pedro; Brogueira, Pedro; Santo, Catarina Espirito; Goncalves, Patricia; Pimenta, Mario; De Angelis, Alessandro

2014-01-01T23:59:59.000Z

343

On The Origin of Very High Energy Cosmic Rays  

E-Print Network (OSTI)

We discuss the most recent developments in our understanding of the acceleration and propagation of cosmic rays up to the highest energies. In particular we specialize our discussion to three issues: 1) developments in the theory of particle acceleration at shock waves; 2) the transition from galactic to extragalactic cosmic rays; 3) implications of up-to-date observations for the origin of ultra high energy cosmic rays (UHECRs).

Pasquale Blasi

2005-11-08T23:59:59.000Z

344

A Fast Gridded Method for the Estimation of the Power Spectrum of the CMB from Interferometer Data with Application to the Cosmic Background Imager  

E-Print Network (OSTI)

We describe an algorithm for the extraction of the angular power spectrum of an intensity field, such as the cosmic microwave background (CMB), from interferometer data. This new method, based on the gridding of interferometer visibilities in the aperture plane followed by a maximum likelihood solution for bandpowers, is much faster than direct likelihood analysis of the visibilities, and deals with foreground radio sources, multiple pointings, and differencing. The gridded aperture-plane estimators are also used to construct Wiener-filtered images using the signal and noise covariance matrices used in the likelihood analysis. Results are shown for simulated data. The method has been used to determine the power spectrum of the cosmic microwave background from observations with the Cosmic Background Imager, and the results are given in companion papers.

S. T. Myers; C. R. Contaldi; J. R. Bond; U. -L. Pen; D. Pogosyan; S. Prunet; J. L. Sievers; B. S. Mason; T. J. Pearson; A. C. S. Readhead; M. C. Shepherd

2002-05-23T23:59:59.000Z

345

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)  

ScienceCinema (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

2011-11-03T23:59:59.000Z

346

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)  

ScienceCinema (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

2011-11-03T23:59:59.000Z

347

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  

SciTech Connect

'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 ) [Director, Center for Energy Efficient Materials; CEEM Staff

2011-05-01T23:59:59.000Z

348

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  

ScienceCinema (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

2011-11-02T23:59:59.000Z

349

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)  

ScienceCinema (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

2011-11-02T23:59:59.000Z

350

Sub-degree Scale Microwave Anisotropies from Cosmic Defects  

E-Print Network (OSTI)

If current ideas about unified field theories are correct, macroscopic cosmic defects may well exist. The observation of such an entity would have enormous significance for our understanding of fundamental physics. This paper points out a novel observable signature of cosmic texture and global monopoles, namely strong hot spots in the cosmic microwave anisotropy pattern on subdegree scales. This signal should be readily detectable by the next generation of anisotropy mapping experiments. The signature arises from overdensities in the photon-baryon fluid generated by the gravitational attraction of the defects. The angular power spectrum of the anisotropy fluctuations on subdegree scales is also calculated, for cosmic string, global monopoles, and texture.

Neil Turok

1996-06-16T23:59:59.000Z

351

Smoothing of the cosmic background radiation by multiple gravitational scattering  

Science Journals Connector (OSTI)

We investigated the smoothing of the cosmic background radiation (CBR) ... rays increases exponentially through multiple scatterings. This exponential growth occurs if the distance is smaller...

Junichiro Making

1994-01-01T23:59:59.000Z

352

The Hubble Web: The Dark Matter Problem and Cosmic Strings  

SciTech Connect

I propose a reinterpretation of cosmic dark matter in which a rigid network of cosmic strings formed at the end of inflation. The cosmic strings fulfill three functions: At recombination they provide an accretion mechanism for virializing baryonic and warm dark matter into disks. These cosmic strings survive as configurations which thread spiral and elliptical galaxies leading to the observed flatness of rotation curves and the Tully-Fisher relation. We find a relationship between the rotational velocity of the galaxy and the string tension and discuss the testability of this model.

Alexander, Stephon [Departments of Physics and Astronomy, Institute for Gravity and Geometry, Pennsylvania State University, University Park, PA 16802 (United States)

2009-07-06T23:59:59.000Z

353

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...

354

The origin of ultra high energy cosmic rays  

E-Print Network (OSTI)

We briefly discuss some open problems and recent developments in the investigation of the origin and propagation of ultra high energy cosmic rays (UHECRs).

Pasquale Blasi

2005-12-16T23:59:59.000Z

355

Falaco Solitons, Cosmic Strings in a Swimming Pool  

E-Print Network (OSTI)

Topological defects experimentally induced by rotational dynamics in a continuous media replicate the coherent structure features of cosmic strings as well as hadrons.

R. M. Kiehn

2001-01-25T23:59:59.000Z

356

On the Dynamics of Two Oscillating Cosmic Strings  

Science Journals Connector (OSTI)

We present the spacetime interval of thenonradiated cosmic string oscillating as standing waves.The influence of string oscillations on the dynamics ofa probe...

T. Omarov; L. Chechin

357

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 -

358

Measuring energy efficiency under heterogeneous technologies using a latent class stochastic frontier approach: An application to Chinese energy economy  

Science Journals Connector (OSTI)

Abstract The importance of technology heterogeneity in estimating economy-wide energy efficiency has been emphasized by recent literature. Some studies use the metafrontier analysis approach to estimate energy efficiency. However, for such studies, some reliable priori information is needed to divide the sample observations properly, which causes a difficulty in unbiased estimation of energy efficiency. Moreover, separately estimating group-specific frontiers might lose some common information across different groups. In order to overcome these weaknesses, this paper introduces a latent class stochastic frontier approach to measure energy efficiency under heterogeneous technologies. An application of the proposed model to Chinese energy economy is presented. Results show that the overall energy efficiency of China's provinces is not high, with an average score of 0.632 during the period from 1997 to 2010.

Boqiang Lin; Kerui Du

2014-01-01T23:59:59.000Z

359

Changes in Energy Intensity 1985-1991  

Gasoline and Diesel Fuel Update (EIA)

Changes in Energy Intensity Changes in Energy Intensity 1985-1991 Overview Full Report The focus is on intensity of energy use measured by energy consumption relative to constant...

360

The New Energy Management Frontier: The Critical Role of a Systematic Management Approach in Making Technology Improvements Successful  

E-Print Network (OSTI)

The New Energy Management Frontier: The Critical Role of a Systematic Management Approach in Making Technology Improvements Successful Jon Feldman Senior Consultant Hatch Consulting Mississauga, Ontario, Canada ABSTRACT Improvements... in technology certainly playa pivotal role in the quest for increased energy efficiency. However, sophisticated industrial energy users are increasingly learning that technology alone cannot drive long-tenn, sustainable reductions in energy cost. The role...

Feldman, J.

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

Intensive Skills Activities CAREERS SERVICE  

E-Print Network (OSTI)

in the state under the cover of night and in broad daylight, perhaps swimming in ship ballast water, tucked and the rest of the world focus more intensely on producing fuels and energy from grasses and other non to subscribe (it's free!), send a note to Futures Editor, 109 Agriculture Hall, Michigan State University, East

Bristol, University of

362

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

363

E-Print Network 3.0 - all-sky cosmic explorer Sample Search Results  

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

monitor with sharp timing capability. This proved decisive in demonstrating that gamma ray... Chapter 8 Cosmic Rays 8.1 Composition and energy distribution Cosmic rays can be...

364

E-Print Network 3.0 - assumed cosmic ray-modulated Sample Search...  

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

Morphology of Anomalous Cosmic Rays in the Outer Heliosphere Summary: ray transport equation describes the physics of cosmic ray modulation in the heliosphere... in this equation...

365

Cosmic string scaling in flat space  

Science Journals Connector (OSTI)

We investigate the evolution of infinite strings as a part of a complete cosmic string network in flat space. We perform a simulation of the network which uses functional forms for the string position and thus is exact to the limits of computer arithmetic. Our results confirm that the wiggles on the strings obey a scaling law described by universal power spectrum. The average distance between long strings also scales accurately with the time. These results suggest that small-scale structure will also scale in an expanding universe, even in the absence of gravitational damping.

Vitaly Vanchurin; Ken Olum; Alexander Vilenkin

2005-09-29T23:59:59.000Z

366

Second Order Geodesic Corrections to Cosmic Shear  

E-Print Network (OSTI)

We consider the impact of second order corrections to the geodesic equation governing gravitational lensing. We start from the full second order metric, including scalar, vector and tensor perturbations, and retain all relevant contributions to the cosmic shear corrections that are second order in the gravitational potential. The relevant terms are: the nonlinear evolution of the scalar gravitational potential, the Born correction, and lens-lens coupling. No other second order terms contribute appreciably to the lensing signal. Since ray-tracing algorithims currently include these three effects, this derivation serves as rigorous justification for the numerical predictions.

S. Dodelson; E. W. Kolb; S. Matarrese; A. Riotto; P. Zhang

2005-03-07T23:59:59.000Z

367

New physics from the Cosmic Microwave Background  

E-Print Network (OSTI)

I review the present status of the Cosmic Microwave Background, with some emphasis on the current and future implications for particle physics. Conclusions are: gravitational instability in a dark matter dominated universe grew today's structure; the Universe remained neutral until z<~50; the CMB power spectrum peaks at 150<~l<~350; the large-scale structure of spacetime appears to be simple; something like inflation is something like proven; we will learn a great deal about cosmology, astrophysics and particle physics from MAP and Planck.

Douglas Scott

1999-11-17T23:59:59.000Z

368

Cosmic Microwave Background Tests of Inflation  

E-Print Network (OSTI)

Inflation provides a unified paradigm for understanding the isotropy of the cosmic microwave background (CMB), the flatness problem, and the origin of large-scale structure. Although the physics responsible for inflation is not yet well understood, slow-roll inflation generically makes several predictions: a flat Universe, primordial adiabatic density perturbations, and a stochastic gravity-wave background. Inflation further predicts specific relations between the amplitudes and shapes of the spectrum of density perturbations and gravity waves. There are now excellent prospects for testing precisely these predictions with forthcoming CMB temperature and polarization maps. Here I discuss these new CMB tests of inflation.

Marc Kamionkowski

1998-03-14T23:59:59.000Z

369

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

370

Gravity, Cosmic Rays and the LHC  

E-Print Network (OSTI)

The high energy proton beams expected when the Large Hadron Collider (LHC) comes online should provide a pass/fail test for a gravity-related explanation of ultrahigh energy cosmic rays. The model predicts that particles have two kinds energies, equal for null gravitational potentials and, in the potential at the Earth, differing significantly above one TeV. If correct, a 7 TeV trajectory energy proton at the LHC would deliver a 23.5 TeV particle state energy in a collision.

Richard Shurtleff

2008-01-20T23:59:59.000Z

371

Origin of the High Energy Cosmic Neutrino Background  

Science Journals Connector (OSTI)

The diffuse background of very high energy extraterrestrial neutrinos recently discovered with IceCube is compatible with that expected from cosmic ray interactions in the Galactic interstellar medium plus that expected from hadronic interactions near the source and in the intergalactic medium of the cosmic rays which have been accelerated by the jets that produce gamma ray bursts.

Shlomo Dado and Arnon Dar

2014-11-07T23:59:59.000Z

372

An electronic radiation of blackbody: Cosmic electron background  

E-Print Network (OSTI)

The Universe owns the electronic radiation of blackbody at temperature 2.725 K, which we call the cosmic electron background. We calculate its radiation spectrum. The energy distribution of number density of electrons in the cosmic electron background becomes zero as energy goes to both zero and infinity. It has one maximum peak near the energy level of 10**(-23) J.

Jian-Miin Liu

2008-02-23T23:59:59.000Z

373

Neutrino physics with an intense \  

E-Print Network (OSTI)

We study some of the physics potential of an intense $1\\,\\mathrm{MCi}$ $^{51}\\mathrm{Cr}$ source combined with the {\\sc Majorana Demonstrator} enriched germanium detector array. The {\\sc Demonstrator} will consist of detectors with ultra-low radioactive backgrounds and extremely low energy thresholds of~$\\sim 400\\,\\mathrm{eV}$. We show that it can improve the current limit on the neutrino magnetic dipole moment. We briefly discuss physics applications of the charged-current reaction of the $^{51}\\mathrm{Cr} neutrino with the $^{73}\\mathrm{Ge} isotope. Finally, we argue that the rate from a realistic, intense tritium source is below the detectable limit of even a tonne-scale HPGe experiment

R. Henning

2010-11-16T23:59:59.000Z

374

29th International Cosmic Ray Conference Pune (2005) 00, 101106 First Estimate of the Primary Cosmic Ray Energy Spectrum  

E-Print Network (OSTI)

Cosmic Ray Energy Spectrum above 3 EeV from the Pierre Auger Observatory The Pierre Auger Collaboration forerunner experiments. A measurement of the cosmic ray energy spectrum in the southern sky is reported here in Argentina now covers an area of approx- imately 1500 km2 . On good-weather nights, air fluorescence

375

28th International Cosmic Ray Conference 4065 The Cosmic Ray Shadows of the Moon and the Sun De-  

E-Print Network (OSTI)

28th International Cosmic Ray Conference 4065 The Cosmic Ray Shadows of the Moon and the Sun De of the data shows that the shadows of the sun and moon have each been detected with high significances of the sun is significantly weaker than that of the moon. As expected, the measured positions of the deficits

California at Santa Cruz, University of

376

Dwarf Galaxies and the Cosmic Web  

Science Journals Connector (OSTI)

We use a cosmological simulation of the formation of the Local Group of Galaxies to identify a mechanism that enables the removal of baryons from low-mass halos without appealing to feedback or reionization. As the Local Group forms, matter bound to it develops a network of filaments and pancakes. This moving web of gas and dark matter drifts and sweeps a large volume, overtaking many halos in the process. The dark matter content of these halos is unaffected but their gas can be efficiently removed by ram pressure. The loss of gas is especially pronounced in low-mass halos due to their lower binding energy and has a dramatic effect on the star formation history of affected systems. This "cosmic web stripping" may help to explain the scarcity of dwarf galaxies compared with the numerous low-mass halos expected in ?CDM and the large diversity of star formation histories and morphologies characteristic of faint galaxies. Although our results are based on a single high-resolution simulation, it is likely that the hydrodynamical interaction of dwarf galaxies with the cosmic web is a crucial ingredient so far missing from galaxy formation models.

Alejandro Bentez-Llambay; Julio F. Navarro; Mario G. Abadi; Stefan Gottlber; Gustavo Yepes; Yehuda Hoffman; Matthias Steinmetz

2013-01-01T23:59:59.000Z

377

Cosmic Acceleration, Dark Energy and Fundamental Physics  

E-Print Network (OSTI)

A web of interlocking observations has established that the expansion of the Universe is speeding up and not slowing, revealing the presence of some form of repulsive gravity. Within the context of general relativity the cause of cosmic acceleration is a highly elastic (p\\sim -rho), very smooth form of energy called ``dark energy'' accounting for about 75% of the Universe. The ``simplest'' explanation for dark energy is the zero-point energy density associated with the quantum vacuum; however, all estimates for its value are many orders-of-magnitude too large. Other ideas for dark energy include a very light scalar field or a tangled network of topological defects. An alternate explanation invokes gravitational physics beyond general relativity. Observations and experiments underway and more precise cosmological measurements and laboratory experiments planned for the next decade will test whether or not dark energy is the quantum energy of the vacuum or something more exotic, and whether or not general relativity can self consistently explain cosmic acceleration. Dark energy is the most conspicuous example of physics beyond the standard model and perhaps the most profound mystery in all of science.

Michael S. Turner; Dragan Huterer

2007-06-26T23:59:59.000Z

378

DWARF GALAXIES AND THE COSMIC WEB  

SciTech Connect

We use a cosmological simulation of the formation of the Local Group of Galaxies to identify a mechanism that enables the removal of baryons from low-mass halos without appealing to feedback or reionization. As the Local Group forms, matter bound to it develops a network of filaments and pancakes. This moving web of gas and dark matter drifts and sweeps a large volume, overtaking many halos in the process. The dark matter content of these halos is unaffected but their gas can be efficiently removed by ram pressure. The loss of gas is especially pronounced in low-mass halos due to their lower binding energy and has a dramatic effect on the star formation history of affected systems. This 'cosmic web stripping' may help to explain the scarcity of dwarf galaxies compared with the numerous low-mass halos expected in {Lambda}CDM and the large diversity of star formation histories and morphologies characteristic of faint galaxies. Although our results are based on a single high-resolution simulation, it is likely that the hydrodynamical interaction of dwarf galaxies with the cosmic web is a crucial ingredient so far missing from galaxy formation models.

Benitez-Llambay, Alejandro; Abadi, Mario G. [Observatorio Astronomico, Universidad Nacional de Cordoba, Cordoba X5000BGR (Argentina); Navarro, Julio F. [Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2 (Canada); Gottloeber, Stefan; Steinmetz, Matthias [Leibniz Institute for Astrophysics, An der Sternwarte 16, D-14482 Potsdam (Germany); Yepes, Gustavo [Departamento de Fisica Teorica, Universidad Autonoma de Madrid, E-28049 Madrid (Spain); Hoffman, Yehuda [Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904 (Israel)

2013-02-01T23:59:59.000Z

379

On the physical basis of cosmic time  

E-Print Network (OSTI)

In this manuscript we initiate a systematic examination of the physical basis for the time concept in cosmology. We discuss and defend the idea that the physical basis of the time concept is necessarily related to physical processes which could conceivably take place among the material constituents available in the universe. It is common practice to link the concept of cosmic time with a space-time metric set up to describe the universe at large scales, and then define a cosmic time $t$ as what is measured by a comoving standard clock. We want to examine, however, the physical basis for setting up a comoving reference frame and, in particular, what could be meant by a standard clock. For this purpose we introduce the concept of a `core' of a clock (which, for a standard clock in cosmology, is a scale-setting physical process) and we ask if such a core can--in principle--be found in the available physics contemplated in the various `stages' of the early universe. We find that a first problem arises above the q...

Rugh, Svend Erik

2008-01-01T23:59:59.000Z

380

Massive Gravity Wrapped in the Cosmic Web  

Science Journals Connector (OSTI)

We study how the filamentary pattern of the cosmic web changes if the true gravity deviates from general relativity (GR) on a large scale. The f(R) gravity, whose strength is controlled to satisfy the current observational constraints on the cluster scale, is adopted as our fiducial model and a large, high-resolution N-body simulation is utilized for this study. By applying the minimal spanning tree algorithm to the halo catalogs from the simulation at various epochs, we identify the main stems of the rich superclusters located in the most prominent filamentary section of the cosmic web and determine their spatial extents per member cluster to be the degree of their straightness. It is found that the f(R) gravity has the effect of significantly bending the superclusters and that the effect becomes stronger as the universe evolves. Even in the case where the deviation from GR is too small to be detectable by any other observables, the degree of the supercluster straightness exhibits a conspicuous difference between the f(R) and the GR models. Our results also imply that the supercluster straightness could be a useful discriminator of f(R) gravity from the coupled dark energy since it is shown to evolve differently between the two models. As a final conclusion, the degree of the straightness of the rich superclusters should provide a powerful cosmological test of large scale gravity.

Junsup Shim; Jounghun Lee; Baojiu Li

2014-01-01T23:59:59.000Z

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381

Theoretical and Experimental Studies of Elementary Particle Physics  

SciTech Connect

The elementary particle physics research program at Indiana University spans a broad range of the most interesting topics in this fundamental field, including important contributions to each of the frontiers identified in the recent report of HEPAP's Particle Physics Prioritization Panel: the Energy Frontier, the Intensity Frontier, and the Cosmic Frontier. Experimentally, we contribute to knowledge at the Energy Frontier through our work on the D0 and ATLAS collaborations. We work at the Intensity Frontier on the MINOS and NOvA experiments and participate in R&D for LBNE. We are also very active on the theoretical side of each of these areas with internationally recognized efforts in phenomenology both in and beyond the Standard Model and in lattice QCD. Finally, although not part of this grant, members of the Indiana University particle physics group have strong involvement in several astrophysics projects at the Cosmic Frontier. Our research efforts are divided into three task areas. The Task A group works on D0 and ATLAS; Task B is our theory group; and Task C contains our MINOS, NOvA, and LBNE (LArTPC) research. Each task includes contributions from faculty, senior scientists, postdocs, graduate and undergraduate students, engineers, technicians, and administrative personnel. This work was supported by DOE Grant DE-FG02-91ER40661. In the following, we describe progress made in the research of each task during the final period of the grant, from November 1, 2009 to April 30, 2013.

Evans, Harold G [Indiana University] [Indiana University; Kostelecky, V Alan [Indiana University] [Indiana University; Musser, James A [Indiana University] [Indiana University

2013-07-29T23:59:59.000Z

382

The effects of coronal mass ejection on galactic cosmic rays in the high latitude heliosphere: Observations from Ulysses` first orbit  

SciTech Connect

During its first solar orbit the Ulysses spacecraft detected several coronal mass ejections (CMEs) at high heliographic latitudes. The authors present first observations on the effects of these high latitude CMEs on galactic cosmic rays (GCRs) using measurements from the Kiel Electron Telescope (KET) which is part of the Cosmic Ray and Solar Particle Investigation (COSPIN) experiment, the Los Alamos SWOOPS (Solar Wind Observations Over the Poles of the Sun) experiment and the magnetic field experiments. They find the passage of these CMEs over the spacecraft to be associated with short term decreases of GCR intensities The relatively weak shocks in these events, driven by the CMEs` over-expansion, had no strong influence on the GCRs. The intensity minimums of GCRs occurred on closed magnetic field lines inside the CMEs themselves as indicated by bidirectional fluxes of suprathermal electrons. Short episodes of intensity increases of GCRs inside CMEs at times when the bidirectional fluxes of suprathermal electrons disappeared, can be interpreted as evidence that GCRs can easily access the interior of those CMEs in which open magnetic field lines are embedded.

Bothmer, V.; Heber, B.; Kunow, H.; Mueller-Mellin, R.; Wibberenz, G. [Univ. of Kiel (Germany). Institut fuer Kernphysik; Gosling, J.T. [Los Alamos National Lab., NM (United States); Balogh, A. [Imperial College, London (United Kingdom). Blackett Lab.; Raviart, A. [CEA, Gif-sur-Yvette (France). Service d`Astrophysique; Paizis, C. [Univ. di Milano (Italy). Istituto di Fisica Cosmica CNR

1997-10-01T23:59:59.000Z

383

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)  

ScienceCinema (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

2011-11-02T23:59:59.000Z

384

Imaging large vessels using cosmic-ray muon energy-loss techniques  

Science Journals Connector (OSTI)

Imaging the internal structure of large vessels (220m in diameter) is not possible with most traditional imaging methods. The sheer size renders gamma-ray and other high-energy photon, neutron, electrical and acoustic techniques useless, whilst the use of high-energy accelerators required to produce charged-particles of sufficient energy are impractical in most industrial situations. The use of naturally occurring high-energy (?GeV) cosmic-ray mu-mesons (muons) provides an effective solution to the penetration problem. The problems of low intensity at near-horizontal angles with the cosmic-ray muon flux are addressed by using energy-loss imaging methods. In other methodologies, using charge-particle energy-loss imaging techniques, only a few events are needed compared to many thousands required if attenuation measurements were to be employed. The energies of horizontal cosmic-ray muons are distributed largely between 0.1 and 1000GeV with a mean energy of about 50GeV. Radiation Transport Monte-Carlo methods (GEANT4) have been used to calculate the energy loss for a selection of industrial materials in the energy range of interest. The energy loss of the muons along a ray-sum are modelled and compared to attenuation losses along the ray-sum using energy resolving detectors in coincidence before and after the sample. The energy-loss spectra across different samples are measured, demonstrating that embedded materials can be identified with as few as 10 muons passing through the sample. It is proposed that the imaging modality can be extended into a full tomographic modality allowing material identification within each voxel.

P.M. Jenneson; W.B. Gilboy; S.J.R. Simons; S.J. Stanley; D. Rhodes

2007-01-01T23:59:59.000Z

385

Handbook of Pediatric Intensive Care  

Science Journals Connector (OSTI)

...objectionable, but I found that it streamlined the text. This handbook is useful in at least two ways. First, it can serve as a mini-textbook on pediatric intensive care. It is not meant to be a substitute for any of the major works in the field, but it does provide enough information for the reader to gain more... In caring for critically ill children, the demands on one's time are great, and there is often little time left for reading. Although there are a number of excellent, comprehensive books on pediatric critical care that must be read by those in the field, ...

Trager J.D.K.

1996-01-25T23:59:59.000Z

386

Energy spectrum of cosmic ray muons in ?100TeV energy region reconstructed from the BUST data  

Science Journals Connector (OSTI)

Inclusive differential and integral energy spectra of cosmic ray muons in the energy range from several TeV to ?1PeV obtained by means of the analysis of multiple interactions of muons (pair meter technique) in the Baksan underground scintillation telescope (BUST) are presented. The results are compared with preceding BUST data on muon energy spectrum based on electromagnetic cascade shower measurements and depth-intensity curve analysis, with calculations for different muon spectrum models, and also with data of other experiments.

A.G. Bogdanov; R.P. Kokoulin; Yu.F. Novoseltsev; R.V. Novoseltseva; V.B. Petkov; A.A. Petrukhin

2012-01-01T23:59:59.000Z

387

Bounds on the density of sources of ultra-high energy cosmic rays from the Pierre Auger Observatory  

SciTech Connect

We derive lower bounds on the density of sources of ultra-high energy cosmic rays from the lack of significant clustering in the arrival directions of the highest energy events detected at the Pierre Auger Observatory. The density of uniformly distributed sources of equal intrinsic intensity was found to be larger than ? (0.06?5) 10{sup ?4} Mpc{sup ?3} at 95% CL, depending on the magnitude of the magnetic deflections. Similar bounds, in the range (0.2?7) 10{sup ?4} Mpc{sup ?3}, were obtained for sources following the local matter distribution.

Collaboration: Pierre Auger Collaboration

2013-05-01T23:59:59.000Z

388

On the ultra high energy cosmic rays and the origin of the cosmic microwave background radiation  

E-Print Network (OSTI)

Some inconsistencies to the assumption of a cosmological origin of the cosmic microwave background CMB, such as the absence of gravitational lensing in the WMAP data, open the doors to some speculations such as a local origin to the CMB. We argue here that this assumption agrees with the absence of the GZK cutoff (at least according to AGASA data) in the energy spectrum of the cosmic ray due to the cosmic interaction with the CMB at $6\\times 10^{19} eV$ or above. Within 50 Mpc from Earth, the matter and light distributions are close to an anisotropic distribution, where the local cluster and local super-clusters of galaxies can be identified. In contrast, the ultra high energy comic rays data is consistent to an almost isotropic distribution, and there is no correlation between their arrival direction and astronomical sources within our local cluster. This means that the events above the GZK cutoff come from distances above 50 Mpc, without an apparent energy loss. This scenario is plausible under the assumption of the CMB concentrated only within 3-4 Mpc from Earth. In other words, the CMB has a local origin linked only to the local super-cluster of galaxies. In addition, the galactic and extragalactic energy spectra index within the energy equipartition theorem strongly constrains the dark matter and dark energy hypothesis, essential in the Big Bang cosmology.

C. E. Navia; C. R. A. Augusto; K. H. Tsui

2007-07-12T23:59:59.000Z

389

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 centers 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 centers 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

390

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

SciTech Connect

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

2011-05-25T23:59:59.000Z

391

NON-EQUILIBRIUM DYNAMICS OF MANY-BODY QUANTUM SYSTEMS: FUNDAMENTALS AND NEW FRONTIER  

SciTech Connect

Rapid progress in nanotechnology and naofabrication techniques has ushered in a new era of quantum transport experiments. This has in turn heightened the interest in theoretical understanding of nonequilibrium dynamics of strongly correlated quantum systems. This project has advanced the frontiers of understanding in this area along several fronts. For example, we showed that under certain conditions, quantum impurities out of equilibrium can be reformulated in terms of an effective equilibrium theory; this makes it possible to use the gamut of tools available for quantum systems in equilibrium. On a different front, we demonstrated that the elastic power of a transmitted microwave photon in circuit QED systems can exhibit a many-body Kondo resonance. We also showed that under many circumstances, bipartite fluctuations of particle number provide an effective tool for studying many-body physicsparticularly the entanglement properties of a many-body system. This implies that it should be possible to measure many-body entanglement in relatively simple and tractable quantum systems. In addition, we studied charge relaxation in quantum RC circuits with a large number of conducting channels, and elucidated its relation to Kondo models in various regimes. We also extended our earlier work on the dynamics of driven and dissipative quantum spin-boson impurity systems, deriving a new formalism that makes it possible to compute the full spin density matrix and spin-spin correlation functions beyond the weak coupling limit. Finally, we provided a comprehensive analysis of the nonequilibrium transport near a quantum phase transition in the case of a spinless dissipative resonant-level model. This project supported the research of two Ph.D. students and two postdoctoral researchers, whose training will allow them to further advance the field in coming years.

DeMille, David; LeHur, Karyn

2013-11-27T23:59:59.000Z

392

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

SciTech Connect

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

393

An Estimate of the Spectral Intensity Expected from the Molecular Bremsstrahlung Radiation in Extensive Air Showers  

E-Print Network (OSTI)

A detection technique of ultra-high energy cosmic rays, complementary to the fluorescence technique, would be the use of the molecular Bremsstrahlung radiation emitted by low-energy electrons left after the passage of the showers in the atmosphere. The emission mechanism is expected from quasi-elastic collisions of electrons produced in the shower by the ionisation of the molecules in the atmosphere. In this article, a detailed calculation of the spectral intensity of photons at ground level originating from the transitions between unquantised energy states of free ionisation electrons is presented. In the absence of absorption of the emitted photons in the plasma, the obtained spectral intensity is shown to be 5 10^{-26} W m^{-2}Hz^{-1} at 10 km from the shower core for a vertical shower induced by a proton of 10^{17.5} eV.

Samarai, I Al; Lebrun, D; Letessier-Selvon, A; Salamida, F

2014-01-01T23:59:59.000Z

394

Gravitational-Wave Stochastic Background from Cosmic Strings  

Science Journals Connector (OSTI)

We consider the stochastic background of gravitational waves produced by a network of cosmic strings and assess their accessibility to current and planned gravitational wave detectors, as well as to big bang nucleosynthesis (BBN), cosmic microwave background (CMB), and pulsar timing constraints. We find that current data from interferometric gravitational wave detectors, such as Laser Interferometer Gravitational Wave Observatory (LIGO), are sensitive to areas of parameter space of cosmic string models complementary to those accessible to pulsar, BBN, and CMB bounds. Future more sensitive LIGO runs and interferometers such as Advanced LIGO and Laser Interferometer Space Antenna (LISA) will be able to explore substantial parts of the parameter space.

Xavier Siemens; Vuk Mandic; Jolien Creighton

2007-03-13T23:59:59.000Z

395

A New Measurement of the Cosmic X-ray Background  

SciTech Connect

I present a new analytical description of the cosmic X-ray background (CXRB) spectrum in the 1.5-200 keV energy band, obtained by combining the new measurement performed by the Swift X-ray telescope (XRT) with the recently published Swift burst alert telescope (BAT) measurement. A study of the cosmic variance in the XRT band (1.5-7 keV) is also presented. I find that the expected cosmic variance (expected from LogN-LogS) scales as {omega}{sup -0.3}(where {omega} is the surveyed area) in very good agreement with XRT data.

Moretti, A. [INAF-Osservatorio Astronomico di Brera v. E. Bianchi 46 23807 Merate (Italy)

2009-05-11T23:59:59.000Z

396

The Cosmic Microwave Background: Beyond the Power Spectrum  

E-Print Network (OSTI)

Much recent work on the cosmic microwave background (CMB) has focussed on the angular power spectrum of temperature anisotropies and particularly on the recovery of cosmological parameters from acoustic peaks in the power spectrum. However, there is more that can conceivably be done with CMB measurements. Here I briefly survey a few such ideas: cross-correlation with other cosmic backgrounds as a probe of the density of the Universe; CMB polarization as a gravitational-wave detector; secondary anisotropies and the ionization history of the Universe; tests of alternative-gravity theories; polarization, the Sunyaev-Zeldovich effect, and cosmic variance; and tests for a neutrino mass.

Marc Kamionkowski

1998-09-24T23:59:59.000Z

397

Gravitating non-Abelian cosmic strings  

E-Print Network (OSTI)

In this paper we study regular cosmic string solutions of the non-Abelian Higgs model coupled with the Einstein gravity. In order to do that, we constructed a set of coupled differential ordinary equation. Because there is no closed solution for this set of equations, we solve it numerically. The solutions that we are interested in asymptote to a flat space-time with a planar angle deficit. This model under consideration present two bosonic sectors, besides the non-Abelian gauge one, coupled minimally with the gravitational fields. The two bosonic sectors may present a direct coupling, which plays an important role on the behavior of the matter and gauge fields and also on the behavior on the geometry of the spacetime. We explicitly analyze the behaviors of the energy density and planar angle deficit as function of the energy scale where the gauge symmetry is spontaneously broken and the coupling interaction between the bosonic sectors.

Santo, Antnio de Padua

2015-01-01T23:59:59.000Z

398

Anisotropies in the Cosmic Microwave Background: Theory  

E-Print Network (OSTI)

Anisotropies in the Cosmic Microwave Background (CMB) contain a wealth of information about the past history of the universe and the present values of cosmological parameters. I ouline some of the theoretical advances of the last few years. In particular, I emphasize that for a wide class of cosmological models, theorists can accurately calculate the spectrum to better than a percent. The specturm of anisotropies today is directly related to the pattern of inhomogeneities present at the time of recombination. This recognition leads to a powerful argument that will enable us to distinguish inflationary models from other models of structure formation. If the inflationary models turn out to be correct, the free parameters in these models will be determined to unprecedented accuracy by the upcoming satellite missions.

Scott Dodelson

1997-02-14T23:59:59.000Z

399

Invariance Violation Extends the Cosmic Ray Horizon?  

E-Print Network (OSTI)

We postulate in the present paper that the energy-momentum relation is modified for very high energy particles to violate Lorentz invariance and the speed of photon is changed from the light velocity c. The violation effect is amplified, in a sensitive way to detection, through the modified kinematical constraints on the conservation of energy and momentum, in the absorption process of gamma-rays colliding against photons of longer wavelengths and converting into an electron-positron pair. For gamma-rays of energies higher than 10 TeV, the minimum energy of the soft photons for the reaction and then the absorption mean free path of gamma-rays are altered by orders of magnitude from the ones conventionally estimated. Consideration is similarly applied to high energy cosmic ray protons. The consequences may require the standard assumptions on the maximum distance that very high energy radiation can travel from to be revised.

Kifune, T

1999-01-01T23:59:59.000Z

400

Invariance Violation Extends the Cosmic Ray Horizon ?  

E-Print Network (OSTI)

We postulate in the present paper that the energy-momentum relation is modified for very high energy particles to violate Lorentz invariance and the speed of photon is changed from the light velocity c. The violation effect is amplified, in a sensitive way to detection, through the modified kinematical constraints on the conservation of energy and momentum, in the absorption process of gamma-rays colliding against photons of longer wavelengths and converting into an electron-positron pair. For gamma-rays of energies higher than 10 TeV, the minimum energy of the soft photons for the reaction and then the absorption mean free path of gamma-rays are altered by orders of magnitude from the ones conventionally estimated. Consideration is similarly applied to high energy cosmic ray protons. The consequences may require the standard assumptions on the maximum distance that very high energy radiation can travel from to be revised.

T. Kifune

1999-04-13T23:59:59.000Z

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.


401

Measuring the Cosmic Shear in Fourier Space  

E-Print Network (OSTI)

We propose to measure the weak cosmic shear using the spatial derivatives of the galaxy surface brightness field. The measurement should be carried out in Fourier space, in which the point spread function (PSF) can be transformed to a desired form with multiplications, and the spatial derivatives can be easily measured. This method is mathematically well defined regardless of the galaxy morphology and the form of the PSF, and involves simple procedures of image processing. Furthermore, with high resolution galaxy images, this approach allows one to probe the shape distortions of galaxy substructures, which can potentially provide much more independent shear measurements than the ellipticities of the whole galaxy. We demonstrate the efficiency of this method using computer-generated mock galaxy images.

Jun Zhang

2006-12-06T23:59:59.000Z

402

The Cosmic Battery in Astrophysical Accretion Disks  

E-Print Network (OSTI)

The aberrated radiation pressure at the inner edge of the accretion disk around an astrophysical black hole imparts a relative azimuthal velocity on the electrons with respect to the ions which gives rise to a ring electric current that generates large scale poloidal magnetic field loops. This is the Cosmic Battery established by Contopoulos and Kazanas in 1998. In the present work we perform realistic numerical simulations of this important astrophysical mechanism in advection-dominated accretion flows-ADAF. We confirm the original prediction that the inner parts of the loops are continuously advected toward the central black hole and contribute to the growth of the large scale magnetic field, whereas the outer parts of the loops are continuously diffusing outward through the turbulent accretion flow. This process of inward advection of the axial field and outward diffusion of the return field proceeds all the way to equipartition, thus generating astrophysically significant magnetic fields on astrophysicall...

Contopoulos, Ioannis; Katsanikas, Matthaios

2015-01-01T23:59:59.000Z

403

Scattering off an SO(10) cosmic string  

Science Journals Connector (OSTI)

The scattering of fermions from the Abelian string arising during the phase transition SO(10)?SU(5)Z2 induced by the Higgs field in the 126 representation is studied. Elastic cross sections and baryon-number-violating cross sections due to the coupling to gauge fields in the core of the string are computed by both a first-quantized method and a perturbative second-quantized method. The elastic cross sections are found to be Aharonov-Bohm-type. However, there is a marked asymmetry between the scattering cross sections for left- and right-handed fields. The catalysis cross sections are small, depending on the grand unified scale. If cosmic strings were observed our results could help tie down the underlying gauge group.

Anne-Christine Davis and Rachel Jeannerot

1995-08-15T23:59:59.000Z

404

Microphysics of SO(10) cosmic strings  

Science Journals Connector (OSTI)

We uncover a rich microphysical structure for SO(10) cosmic strings. For the Abelian string the electroweak symmetry is restored around it in a region depending on the electroweak scale. Four distinct non-Abelian strings are found. Some of these also restore the electroweak symmetry. We investigate the zero mode structure of our strings. Whilst there are right-handed neutrino zero modes for the Abelian string, they do not survive the electroweak phase transition in the case of the lowest energy solution. We elucidate the zero mode structure for the non-Abelian strings above and below the electroweak phase transition. We consider the generalization of our results to other theories and consider the cosmological consequences of them.

Anne-Christine Davis and Stephen C. Davis

1997-02-15T23:59:59.000Z

405

End of the cosmic neutrino energy spectrum  

E-Print Network (OSTI)

There may be a high-energy cutoff of neutrino events in IceCube data. In particular, IceCube does not observe the Standard Model Glashow-resonance events expected at 6.3 PeV. There are also no higher-energy neutrino signatures in the ANITA and Auger experiments. This absence of high-energy neutrino events motivates models with a fundamental restriction on neutrino energies above a few PeV. The simplest scenario to terminate the neutrino spectrum is Lorentz-invariance violating with a limiting neutrino velocity that is smaller than the speed of light. A consequence is that charged pions are stable above four times the maximum neutrino energy and may serve as a cosmic ray primary.

Anchordoqui, L A; Goldberg, H; Learned, J G; Marfatia, D; Pakvasa, S; Paul, T C; Weiler, T J

2014-01-01T23:59:59.000Z

406

Information Gains from Cosmic Microwave Background Experiments  

E-Print Network (OSTI)

To shed light on the fundamental problems posed by Dark Energy and Dark Matter, a large number of experiments have been performed and combined to constrain cosmological models. We propose a novel way of quantifying the information gained by updates on the parameter constraints from a series of experiments which can either complement earlier measurements or replace them. For this purpose, we use the Kullback-Leibler divergence or relative entropy from information theory to measure differences in the posterior distributions in model parameter space from a pair of experiments. We apply this formalism to a historical series of Cosmic Microwave Background experiments ranging from Boomerang to WMAP, SPT, and Planck. Considering different combinations of these experiments, we thus estimate the information gain in units of bits and distinguish contributions from the reduction of statistical errors and the `surprise' corresponding to a significant shift of the parameters' central values. For this experiment series, we...

Seehars, Sebastian; Refregier, Alexandre; Paranjape, Aseem; Akeret, Jol

2014-01-01T23:59:59.000Z

407

Coherence and oscillations of cosmic neutrinos  

E-Print Network (OSTI)

For cosmic neutrinos we study the conditions and the effects of the coherence loss as well as coherent broadening of the spectrum. We evaluate the width of the neutrino wavepacket produced by charged particles under various circumstances: in an interaction-free environment, in a radiation-dominated medium (typical of the sources of the gamma ray bursts) and in the presence of a magnetic field. The effect of the magnetic field on the wavepacket size appears to be more important than the scattering. If the magnetic field at the source is larger than $\\sim$10 Gauss, the coherence of neutrinos will be lost while traveling over cosmological distances. Various applications of these results have been considered. We find that for large magnetic fields ($B> 10^9$ Gauss) and high energies ($E_\

Yasaman Farzan; Alexei Yu Smirnov

2008-03-04T23:59:59.000Z

408

Gravitational waves from cosmic bubble collisions  

E-Print Network (OSTI)

Cosmic bubbles are nucleated through the quantum tunneling process. After nucleation they would expand and undergo collisions with each other. In this paper, we focus in particular on collisions of two equal-sized bubbles and compute gravitational waves emitted from the collisions. First, we study the mechanism of the collisions by means of a real scalar field and a quartic potential of the field. Then, using this scalar field model, we compute gravitational waves from the collisions in a straightforward manner. In the quadrupole approximation, time-domain gravitational waveforms are directly obtained by integrating the energy-momentum tensors over the volume of the wave sources, where the energy-momentum tensors are expressed in terms of the scalar field, the local geometry and the potential; therefore, containing all information about the bubble collisions. We present gravitational waveforms emitted during (i) the initial-to-intermediate stage of strong collisions and (ii) the final stage of weak collisions...

Kim, Dong-Hoon; Lee, Wonwoo; Yang, Jongmann; Yeom, Dong-han

2014-01-01T23:59:59.000Z

409

The `excess' of primary cosmic ray electrons  

E-Print Network (OSTI)

With the accurate cosmic ray (CR) electron and positron spectra (denoted as $\\Phi_{\\rm e^{-}}$ and $\\Phi_{\\rm e^{+}}$, respectively) measured by AMS-02 collaboration, the difference between the electron and positron fluxes (i.e., $\\Delta \\Phi=\\Phi_{\\rm e^{-}}-\\Phi_{\\rm e^{+}}$), dominated by the propagated primary electrons, can be reliably inferred. In the standard model, the spectrum of propagated primary CR electrons at energies $\\geq 30$ GeV softens with the increase of energy. The absence of any evidence for such a continuous spectral softening in $\\Delta \\Phi$ strongly suggests a significant `excess' of primary CR electrons and at energies of $100-400$ GeV the identified excess component has a flux comparable to that of the observed positron excess. Middle-age but `nearby' supernova remnants (e.g., Monogem and Geminga) are favored sources for such an excess.

Li, Xiang; Lu, Bo-Qiang; Dong, Tie-Kuang; Fan, Yi-Zhong; Feng, Lei; Liu, Si-Ming; Chang, Jin

2014-01-01T23:59:59.000Z

410

Processing of formic acid-containing ice by heavy and energetic cosmic ray analogues  

E-Print Network (OSTI)

Formic acid (HCOOH) has been extensively detected in space environments, including interstellar medium (gas and grains), comets and meteorites. Such environments are often subjected to the action of ionizing agents, which may cause changes in the molecular structure, thus leading to formation of new species. Formic acid is a possible precursor of pre-biotic species, such as Glycine (NH2CH2COOH). This work investigates experimentally the physicochemical effects resulting from interaction of heavy and energetic cosmic ray analogues (46MeV 58Ni11+) in H2O:HCOOH (1:1) ice, at 15 K, in ultrahigh vacuum regime, using Fourier transform infrared spectrometry in the mid-infrared region (4000-600 cm-1 or 2.5-12.5 microns). After the bombardment, the sample was slowly heated to room temperature. The results show the dissociation cross-section for the formic acid of 2.4x10^-13 cm2, and half-life due to galactic cosmic rays of 8x10^7 yr. The IR spectra show intense formation of CO and CO2, and small production of more com...

Bergantini, A; Rothard, H; Boduch, P; Andrade, D P P

2014-01-01T23:59:59.000Z

411

On the physical basis of cosmic time  

E-Print Network (OSTI)

In this manuscript we initiate a systematic examination of the physical basis for the time concept in cosmology. We discuss and defend the idea that the physical basis of the time concept is necessarily related to physical processes which could conceivably take place among the material constituents available in the universe. It is common practice to link the concept of cosmic time with a space-time metric set up to describe the universe at large scales, and then define a cosmic time $t$ as what is measured by a comoving standard clock. We want to examine, however, the physical basis for setting up a comoving reference frame and, in particular, what could be meant by a standard clock. For this purpose we introduce the concept of a `core' of a clock (which, for a standard clock in cosmology, is a scale-setting physical process) and we ask if such a core can--in principle--be found in the available physics contemplated in the various `stages' of the early universe. We find that a first problem arises above the quark-gluon phase transition (which roughly occurs when the cosmological model is extrapolated back to $\\sim 10^{-5}$ seconds) where there might be no bound systems left, and the concept of a physical length scale to a certain extent disappears. A more serious problem appears above the electroweak phase transition believed to occur at $\\sim 10^{-11}$ seconds. At this point the property of mass (almost) disappears and it becomes difficult to identify a physical basis for concepts like length scale, energy scale and temperature -- which are all intimately linked to the concept of time in modern cosmology. This situation suggests that the concept of a time scale in `very early' universe cosmology lacks a physical basis or, at least, that the time scale will have to be based on speculative new physics.

Svend Erik Rugh; Henrik Zinkernagel

2008-05-13T23:59:59.000Z

412

Towards an understanding of the rapid decline of the cosmic star formation rate  

E-Print Network (OSTI)

We present a first analysis of deep 24 micron observations with the Spitzer Space Telescope of a sample of nearly 1500 galaxies in a thin redshift slice, 0.65projects. To characterize the decline in star-formation rate (SFR) since z~0.7, we estimate the total thermal infrared (IR) luminosities, SFRs, and stellar masses for the galaxies in this sample. At z~0.7, nearly 40% of intermediate and high-mass galaxies (with stellar masses >2x10^10 solar masses) are undergoing a period of intense star formation above their past-averaged SFR. In contrast, less than 1% of equally-massive galaxies in the local universe have similarly intense star formation activity. Morphologically-undisturbed galaxies dominate the total infrared luminosity density and SFR density: at z~0.7, more than half of the intensely star-forming galaxies have spiral morphologies, whereas less than \\~30% are strongly interacting. Thus, a decline in major-merger rate is not the underlying cause of the rapid decline in cosmic SFR since z~0.7. Physical properties that do not strongly affect galaxy morphology - for example, gas consumption and weak interactions with small satellite galaxies - appear to be responsible.

Eric F. Bell; Casey Papovich; Christian Wolf; Emeric Le Floc'h; John A. R. Caldwell; Marco Barden; Eiichi Egami; Daniel H. McIntosh; Klaus Meisenheimer; Pablo G. P. Perez-Gonzalez; George H. Rieke; Marcia J. Rieke; Jane R. Rigby; Hans-Walter Rix

2005-02-11T23:59:59.000Z

413

Effect of a chameleon scalar field on the cosmic microwave background  

Science Journals Connector (OSTI)

We show that a direct coupling between a chameleonlike scalar field and photons can give rise to a modified Sunyaev-Zeldovich (SZ) effect in the cosmic microwave background (CMB). The coupling induces a mixing between chameleon particles and the CMB photons when they pass through the magnetic field of a galaxy cluster. Both the intensity and the polarization of the radiation are modified. The degree of modification depends strongly on the properties of the galaxy cluster such as magnetic field strength and electron number density. Existing SZ measurements of the Coma cluster enable us to place constraints on the photon-chameleon coupling. The constrained conversion probability in the cluster is PComa(204??GHz)<6.210-5 at 95% confidence, corresponding to an upper bound on the coupling strength of geff(cell)<2.210-8??GeV-1 or geff(Kolmo)<(7.232.5)10-10??GeV-1, depending on the model that is assumed for the cluster magnetic field structure. We predict the radial profile of the chameleonic CMB intensity decrement. We find that the chameleon effect extends farther toward the edges of the cluster than the thermal SZ effect. Thus we might see a discrepancy between the x-ray emission data and the observed SZ intensity decrement. We further predict the expected change to the CMB polarization arising from the existence of a chameleonlike scalar field. These predictions could be verified or constrained by future CMB experiments.

Anne-Christine Davis; Camilla A. O. Schelpe; Douglas J. Shaw

2009-09-10T23:59:59.000Z

414

Simulations of reflected radio signals from cosmic ray induced air showers  

E-Print Network (OSTI)

We present the calculation of coherent radio pulses emitted by extensive air showers induced by ultra-high energy cosmic rays accounting for reflection on the Earth's surface. Results have been obtained with a simulation program that calculates the contributions from shower particles after reflection at a surface plane. The properties of the radiation are discussed in detail emphasizing the effects of reflection. The shape of the frequency spectrum is shown to be closely related to the angle of the observer with respect to shower axis, becoming hardest in the Cherenkov direction. The intensity of the flux at a fixed observation angle is shown to scale with the square of the primary particle energy to very good accuracy indicating the coherent aspect of the emission. The simulation methods of this paper provide the foundations for energy reconstruction of experiments looking at the Earth from balloons and satellites. They can also be used in dedicated studies of existing and future experimental proposals.

Alvarez-Muiz, Jaime; Garca-Fernndez, Daniel; Schoorlemmer, Harm; Zas, Enrique

2015-01-01T23:59:59.000Z

415

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

416

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...

417

Cosmic rays, lithium abundance and excess entropy in galaxy clusters  

Science Journals Connector (OSTI)

......elements such as beryllium and boron are not produced during...Anisotropy Probe (WMAP) determination of the cosmic baryon density...mass from the predominant isotope of 7Li, making lines from these two isotopes blend easily. Until recently......

Biman B. Nath; Piero Madau; Joseph Silk

2006-02-01T23:59:59.000Z

418

The cosmic ray muon energy spectum via ?erenkov radiation  

E-Print Network (OSTI)

In this thesis, I designed and constructed a basic Cerenkov detector to measure the energy spectrum of cosmic ray muons for use in the graduate experimental physics courses, 8.811/2. The apparatus consists of a light-tight ...

Quintero, Eric Antonio

2010-01-01T23:59:59.000Z

419

Muons of very and ultra-high energy cosmic rays  

Science Journals Connector (OSTI)

In many cosmic rays experiments at very and ultra-high energies, an excess of muons (including those of very high energy, >100 TeV) is observed that cannot ... compositions, and especially the observed excesses o...

A. G. Bogdanov; R. P. Kokoulin

2013-11-01T23:59:59.000Z

420

Bulk Viscosity, Decaying Dark Matter, and the Cosmic Acceleration  

E-Print Network (OSTI)

We discuss a cosmology in which cold dark-matter particles decay into relativistic particles. We argue that such decays could lead naturally to a bulk viscosity in the cosmic fluid. For decay lifetimes comparable to the present hubble age, this bulk viscosity enters the cosmic energy equation as an effective negative pressure. We investigate whether this negative pressure is of sufficient magnitude to account fo the observed cosmic acceleration. We show that a single decaying species in a flat, dark-matter dominated cosmology without a cosmological constant cannot reproduce the observed magnitude-redshift relation from Type Ia supernovae. However, a delayed bulk viscosity, possibly due to a cascade of decaying particles may be able to account for a significant fraction of the apparent cosmic acceleration. Possible candidate nonrelativistic particles for this scenario include sterile neutrinos or gauge-mediated decaying supersymmetric particles.

James R. Wilson; Grant J. Mathews; George M. Fuller

2006-09-25T23:59:59.000Z

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.


421

Pulsar Wind Nebulae and Cosmic Rays: A Bedtime Story  

E-Print Network (OSTI)

The role pulsar wind nebulae play in producing our locally observed cosmic ray spectrum remains murky, yet intriguing. Pulsar wind nebulae are born and evolve in conjunction with SNRs, which are favored sites of Galactic cosmic ray acceleration. As a result they frequently complicate interpretation of the gamma-ray emission seen from SNRs. However, pulsar wind nebulae may also contribute directly to the local cosmic ray spectrum, particularly the leptonic component. This paper reviews the current thinking on pulsar wind nebulae and their connection to cosmic ray production from an observational perspective. It also considers how both future technologies and new ways of analyzing existing data can help us to better address the relevant theoretical questions. A number of key points will be illustrated with recent results from the VHE (E > 100 GeV) gamma-ray observatory VERITAS.

,

2014-01-01T23:59:59.000Z

422

A Quantum Phase Transition in the Cosmic Ray Energy Distribution  

E-Print Network (OSTI)

We here argue that the "knee" of the cosmic ray energy distribution at $E_c \\sim 1$ PeV represents a second order phase transition of cosmic proportions. The discontinuity of the heat capacity per cosmic ray particle is given by $\\Delta c=0.450196\\ k_B$. However the idea of a deeper critical point singularity cannot be ruled out by present accuracy in neither theory nor experiment. The quantum phase transition consists of cosmic rays dominated by bosons for the low temperature phase E E_c$. The low temperature phase arises from those nuclei described by the usual and conventional collective boson models of nuclear physics. The high temperature phase is dominated by protons. The transition energy $E_c$ may be estimated in terms of the photo-disintegration of nuclei.

Widom, A; Srivastava, Y

2015-01-01T23:59:59.000Z

423

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

424

Energy Intensity Baselining and Tracking Guidance  

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

The Energy Intensity Baselining and Tracking Guidance for the Better Buildings, Better Plants Program helps companies meet the programs reporting requirements by describing the steps necessary to develop an energy consumption and energy intensity baseline and calculating consumption and intensity changes over time.

425

Cosmic Ray Muons Timing in the ATLAS Detector  

Science Journals Connector (OSTI)

In this talk I discuss the use of calorimeter timing both for detector commissioning and in searches for new physics. In particular I present real and simulated cosmic ray muons data (2007) results for the ATLAS Tile Calorimeter system. The analysis shows that several detector errors such as imperfect calibrations can be uncovered. I also demonstrate the use of ATLAS Tile Calorimeters excellent timing resolution in suppressing cosmic ray fake missing transverse energy (E T ) in searches for supersymmetry.

Bernhard Meirose; ATLAS Tile Calorimeter System

2009-01-01T23:59:59.000Z

426

Galactic cosmic rays M.-B. Kallenrode  

E-Print Network (OSTI)

- larities, convection with the solar wind, drifts in the large-scale heliospheric magnetic field intensities. In addition, because of the high variability of the solar wind and the embedded magnetic field we?', `How are they accelerated to such high energies?', and `How do they prop- agate through

Steinhoff, Heinz-Jürgen

427

Division of Environmental Studies, Graduate School of Frontier Sciences, The University of Tokyo Guide to The 2014 Entrance Examination of Master & Doctor Courses and Inquiry Sheet  

E-Print Network (OSTI)

, education, aging societies and information pollution ? Division of Environmental Studies: Background of Environmental Studies moved to a brand-new building in the Kashi- wa Campus and commenced five new departmentsDivision of Environmental Studies, Graduate School of Frontier Sciences, The University of Tokyo

Yamamoto, Hirosuke

428

Mapping the Cosmic Web with Ly? Emission  

Science Journals Connector (OSTI)

We use a high-resolution cosmological simulation to predict the distribution of H I Ly? emission from the low-redshift (z 0.5) intergalactic medium (IGM). Our simulation can be used to reliably compute the emission from optically thin regions of the IGM but not that of self-shielded gas. We therefore consider several models that bracket the expected emission from self-shielded regions. Most galaxies are surrounded by extended (102kpc) "coronae" of optically thin gas with Ly? surface brightness close to the expected background. Most of these regions contain smaller cores of dense, cool gas. Unless self-shielded gas is able to cool to T 4.1 K, these cores are much brighter than the background. The Ly? coronae represent "cooling flows" of IGM gas accreting onto galaxies. We also estimate the number of Ly? photons produced through the reprocessing of stellar ionizing radiation in the interstellar medium of galaxies; while this mechanism is responsible for the brightest Ly? emission, it occurs on small physical scales and can be separated using high-resolution observations. In all cases, we find that Ly? emitters are numerous (with a space density of ~0.1 h3 Mpc-3) and closely trace the filamentary structure of the IGM, providing a new way to map gas inside the cosmic web.

Steven R. Furlanetto; Joop Schaye; Volker Springel; Lars Hernquist

2003-01-01T23:59:59.000Z

429

Statistics of Cosmic Microwave Background Polarization  

E-Print Network (OSTI)

We present a formalism for analyzing a full-sky temperature and polarization map of the cosmic microwave background. Temperature maps are analyzed by expanding over the set of spherical harmonics to give multipole moments of the two-point correlation function. Polarization, which is described by a second-rank tensor, can be treated analogously by expanding in the appropriate tensor spherical harmonics. We provide expressions for the complete set of temperature and polarization multipole moments for scalar and tensor metric perturbations. Four sets of multipole moments completely describe isotropic temperature and polarization correlations; for scalar metric perturbations one set is identically zero, giving the possibility of a clean determination of the vector and tensor contributions. The variance with which the multipole moments can be measured in idealized experiments is evaluated, including the effects of detector noise, sky coverage, and beam width. Finally, we construct coordinate-independent polarization two-point correlation functions, express them in terms of the multipole moments, and derive small-angle limits.

Marc Kamionkowski; Arthur Kosowsky; Albert Stebbins

1996-11-15T23:59:59.000Z

430

THE COSMIC NEAR-INFRARED BACKGROUND. II. FLUCTUATIONS  

SciTech Connect

The near-infrared background (NIRB) is one of a few methods that can be used to observe the redshifted light from early stars at a redshift of 6 and above, and thus it is imperative to understand the significance of any detection or nondetection of the NIRB. Fluctuations of the NIRB can provide information on the first structures, such as halos and their surrounding ionized regions in the intergalactic medium (IGM). We combine, for the first time, N-body simulations, radiative transfer code, and analytic calculations of luminosity of early structures to predict the angular power spectrum (C{sub l} ) of fluctuations in the NIRB. We study in detail the effects of various assumptions about the stellar mass, the initial mass spectrum of stars, the metallicity, the star formation efficiency (f{sub *}), the escape fraction of ionizing photons (f{sub esc}), and the star formation timescale (t{sub SF}), on the amplitude as well as the shape of C{sub l} . The power spectrum of NIRB fluctuations is maximized when f{sub *} is the largest (as C{sub l} {proportional_to} f {sup 2}{sub *}) and f{sub esc} is the smallest (as more nebular emission is produced within halos). A significant uncertainty in the predicted amplitude of C{sub l} exists due to our lack of knowledge of t{sub SF} of these early populations of galaxies, which is equivalent to our lack of knowledge of the mass-to-light ratio of these sources. We do not see a turnover in the NIRB angular power spectrum of the halo contribution, which was claimed to exist in the literature, and explain this as the effect of high levels of nonlinear bias that was ignored in the previous calculations. This is partly due to our choice of the minimum mass of halos contributing to NIRB ({approx}2 x 10{sup 9} M{sub sun}), and a smaller minimum mass, which has a smaller nonlinear bias, may still exhibit a turnover. Therefore, our results suggest that both the amplitude and shape of the NIRB power spectrum provide important information regarding the nature of sources contributing to the cosmic reionization. The angular power spectrum of the IGM, in most cases, is much smaller than the halo angular power spectrum, except when f{sub esc} is close to unity, t{sub SF} is longer, or the minimum redshift at which the star formation is occurring is high. In addition, low levels of the observed mean background intensity tend to rule out high values of f{sub *} {approx}> 0.2.

Fernandez, Elizabeth R. [Center for Astrophysics and Space Astronomy, University of Colorado, 389 UCB, Boulder, CO 80309-0389 (United States); Komatsu, Eiichiro; Shapiro, Paul R. [Texas Cosmology Center and the Department of Astronomy, University of Texas at Austin, 1 University Station, C1400, Austin, TX 78712 (United States); Iliev, Ilian T., E-mail: elizabeth.fernandez@colorado.ed [Astronomy Centre, Department of Physics and Astronomy, Pevensey II Building, University of Sussex, Falmer, Brighton BN1 9QH (United Kingdom)

2010-02-20T23:59:59.000Z

431

New Constraints on Cosmic Polarization Rotation from B-Mode Polarization in Cosmic Microwave Background  

E-Print Network (OSTI)

STPpol, POLARBEAR and BICEP2 have recently measured the cosmic microwave background (CMB) B-mode polarization in various sky regions of several tens of square degrees and obtained BB power spectra in the multipole range 20-3000, detecting the components due to gravitational lensing and to inflationary gravitational waves. We analyze jointly the results of these three experiments and propose modifications of their analysis of the spectra to include in the model, in addition to the gravitational lensing and the inflationary gravitational waves components, also the effects induced by the cosmic polarization rotation (CPR), if it exists within current upper limits. Although in principle our analysis would lead also to new constraints on CPR, in practice these can only be given on its fluctuations , since constraints on its mean angle are inhibited by the de-rotation which is applied by current CMB polarization experiments, in order to cope with the insufficient calibration of the polarization angle. The combined data fits from all three experiments (with 29% CPR-SPTpol correlation, depending on theoretical model) gives constraint ^1/2 areas observed by SPTpol, POLARBEAR and BICEP2.

Sperello di Serego Alighieri; Wei-Tou Ni; Wei-Ping Pan

2014-04-07T23:59:59.000Z

432

Energy Intensity Baselining and Tracking Guidance  

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

Learn more at betterbuildings.energy.gov Energy Intensity Baselining and Tracking Guidance i Preface The U.S. Department of Energy's (DOE) Better Buildings, Better Plants Program...

433

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 heating is a very attractive 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

434

Cosmic and Galactic Neutrino Backgrounds from Thermonuclear Sources  

E-Print Network (OSTI)

We estimate energy spectra and fluxes at the Earth's surface of the cosmic and Galactic neutrino backgrounds produced by thermonuclear reactions in stars. The extra-galactic component is obtained by combining the most recent estimates of the cosmic star formation history and the stellar initial mass function with accurate theoretical predictions of the neutrino yields all over the thermonuclear lifetime of stars of different masses. Models of the structure and evolution of the Milky Way are used to derive maps of the expected flux generated by Galactic sources as a function of sky direction. The predicted neutrino backgrounds depend only slightly on model parameters. In the relevant 50 keV-10 MeV window, the total flux of cosmic neutrinos ranges between 20 and 65 particles per square cm per s. Neutrinos reaching the Earth today have been typically emitted at redshift z~2. Their energy spectrum peaks at E~0.1-0.3 MeV. The energy and entropy densities of the cosmic background are negligible with respect to the thermal contribution of relic neutrinos originated in the early universe. In every sky direction, the cosmic background is outnumbered by the Galactic one, whose integrated flux amounts to 300-1000 particles per square cm per s. The emission from stars in the Galactic disk contributes more than 95 per cent of the signal.

Cristiano Porciani; Silvia Petroni; Giovanni Fiorentini

2003-11-20T23:59:59.000Z

435

World Best Practice Energy Intensity Values for Selected Industrial Sectors  

E-Print Network (OSTI)

world best practice energy intensity values for productionWorld best practice energy intensity values for productionWorld Best Practice Final Energy Intensity Values for Aluminium Production (

Worrell, Ernst; Price, Lynn; Neelis, Maarten; Galitsky, Christina; Zhou, Nan

2007-01-01T23:59:59.000Z

436

World Best Practice Energy Intensity Values for Selected Industrial Sectors  

E-Print Network (OSTI)

Best Practice Final Energy Intensity Values for Stand-AloneBest Practice Final Energy Intensity Values for Stand-AloneBest Practice Primary Energy Intensity Values for Stand-

Worrell, Ernst; Price, Lynn; Neelis, Maarten; Galitsky, Christina; Zhou, Nan

2007-01-01T23:59:59.000Z

437

Expansion and Collapse in the Cosmic Web  

Science Journals Connector (OSTI)

We study the kinematics of the gaseous cosmic web at high redshift using Ly? forest absorption in multiple QSO sight lines. Observations of the projected velocity shifts between Ly? absorbers common to the lines of sight to a gravitationally lensed QSO and three more widely separated QSO pairs are used to directly measure the expansion of the cosmic web in units of the Hubble velocity, as a function of redshift and spatial scale. The lines of sight used span a redshift range from about 2 to 4.5 and represent transverse scales from the subkiloparsec range to about 300 h physical kpc. Using a simple analytic model and a cosmological hydrodynamic simulation, we constrain the underlying three-dimensional distribution of expansion velocities from the observed line-of-sight distribution of velocity shear across the plane of the sky. The shape of the shear distribution and its width (14.9 km s-1 rms for a physical transverse separation of 61 h kpc at z = 2, 30.0 km s-1 for 261 h kpc at z = 3.6) are found to be in good agreement with the IGM undergoing large-scale motions dominated by the Hubble flow, making this one of the most direct observations possible of the expansion of the universe. However, modeling the Ly? clouds with a simple "expanding pancake" model, the average expansion velocity of the gaseous structures causing the Ly? forest in the lower redshift (z ~ 2) smaller separation (61 kpc) sample appears about 20% lower than the local Hubble expansion velocity. In order to understand the observed velocity distribution further we investigated the statistical distribution of expansion velocities in cosmological Ly? forest simulations. The mean expansion velocity in the (z ~ 2, separation ~ 60 kpc) simulation is indeed somewhat smaller than the Hubble velocity, as found in the real data. We interpret this finding as tentative evidence for some Ly? forest clouds breaking away from the Hubble flow and undergoing the early stages of gravitational collapse. However, the distribution of velocities is highly skewed, and the majority of Ly? forest clouds at all redshifts from 2 to 3.8 expand with super-Hubble velocities, typically about 5%-20% faster than the Hubble flow. This behavior is explained if most Ly? forest clouds in the column density range typically detectable are expanding filaments that stretch and drain into more massive nodes. The significant difference seen in the velocity distributions between the high- and low-redshift samples may conceivably reflect actual peculiar deceleration, the differences in spatial scale, or our selecting higher densities at lower redshift for a given detection threshold for Ly? forest lines. We also investigate the alternative possibility that the velocity structure of the general Ly? forest could have an entirely different, local origin, as expected if the Ly? forest were produced or at least significantly modified by galactic feedback, e.g., winds from star-forming galaxies at high redshift. However, we find no evidence that the observed distribution of velocity shear is significantly influenced by processes other than Hubble expansion and gravitational instability. To avoid overly disturbing the IGM, galactic winds may be old and/or limp by the time we observe them in the Ly? forest, or they may occupy only an insignificant volume fraction of the IGM. We briefly discuss the observational evidence usually presented in favor of an IGM afflicted by high-redshift extragalactic superwinds and find much of it ambiguous. During the hierarchical buildup of structure, galaxies are expected to spill parts of their interstellar medium and to heat and stir the IGM in ways that make it hard to disentangle this gravitational process from the effects of winds.

Michael Rauch; George D. Becker; Matteo Viel; Wallace L. W. Sargent; Alain Smette; Robert A. Simcoe; Thomas A. Barlow; Martin G. Haehnelt

2005-01-01T23:59:59.000Z

438

High-energy cosmic-ray muons at ground level and below ground level  

Science Journals Connector (OSTI)

Cosmic-ray muon interactions have been studied in an analysis of very recent measurements of cosmic-ray muons at sea-level and large depths underground ... By starting with the very carefully measured vertical muon

C. R. Paul; N. Chaudhuri

1977-01-11T23:59:59.000Z

439

Extra-terrestrial life in the European Space Agencys Cosmic Vision plan and beyond  

Science Journals Connector (OSTI)

...Royal Society 13 February 2011 review-article Articles 1000 8 71...Space Agencys Cosmic Vision plan and beyond Malcolm Fridlund...programme. Following favourable reviews by ESAs scientific advisory...Space Agency's Cosmic Vision plan and beyond. | Our exciting...

2011-01-01T23:59:59.000Z

440

E-Print Network 3.0 - accelerated cosmic expansion Sample Search...  

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

Groningen Collection: Physics 6 Cosmic Ray Acceleration beyond the Knee up to the Ankle in the Galactic Wind Halo Summary: Cosmic Ray Acceleration beyond the Knee up to the...

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.


441

E-Print Network 3.0 - average solar-cosmic-ray fluxes Sample...  

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

solar-cosmic-ray fluxes Search Powered by Explorit Topic List Advanced Search Sample search results for: average solar-cosmic-ray fluxes Page: << < 1 2 3 4 5 > >> 1 Annales...

442

Astrophysical explosions: from solar flares to cosmic gamma-ray bursts  

Science Journals Connector (OSTI)

...from solar flares to cosmic gamma-ray bursts J. Craig Wheeler * * wheel...collapse supernovae and cosmic gamma-ray bursts, each representing a different...black holes|supernovae|gamma-ray bursts|deflagration|detonation...

2012-01-01T23:59:59.000Z

443

Cosmic Radiation Protection Dosimetry Using an Electronic Personal Dosemeter (Siemens EPD) on Selected International Flights  

Science Journals Connector (OSTI)

......administration to promote radiation safety for air carrier...aircrew to cosmic radiation. Radiat. Prot...1995) EPD Software Version 8: Electronic...Health and Safety Laboratory, New...Physics of cosmic radiation fields. Radiat......

Hiroshi Yasuda; Kazunobu Fujitaka

2001-03-01T23:59:59.000Z

444

Comparison of codes assessing galactic cosmic radiation exposure of aircraft crew  

Science Journals Connector (OSTI)

......the galactic cosmic radiation. Results are provided...fully satisfactory for radiation protection purposes...Protection and Nuclear Safety, F-92262 Fontenay-aux-Roses...Computer Simulation Cosmic Radiation Europe Humans Occupational...instrumentation methods Software Solar Activity...

J. F. Bottollier-Depois; P. Beck; B. Bennett; L. Bennett; R. Btikofer; I. Clairand; L. Desorgher; C. Dyer; E. Felsberger; E. Flckiger; A. Hands; P. Kindl; M. Latocha; B. Lewis; G. Leuthold; T. Maczka; V. Mares; M. J. McCall; K. O'Brien; S. Rollet; W. Rhm; F. Wissmann

2009-10-01T23:59:59.000Z

445

E-Print Network 3.0 - alternative high-z cosmic Sample Search...  

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

5 > >> 1 StructureStructure in the Universein the Universe Summary: -rays Gaseous Cosmic Web - Baryonic gas traces the Cosmic Web: Ly forest neutral hydrogen gas, mostly at high...

446

COSMIC RAY HEATING OF THE WARM IONIZED MEDIUM  

SciTech Connect

Observations of line ratios in the Milky Way's warm ionized medium suggest that photoionization is not the only heating mechanism present. For the additional heating to explain the discrepancy, it would have to have a weaker dependence on the gas density than the cooling rate, {Lambda}n{sub e}{sup 2}. Reynolds et al. suggested turbulent dissipation or magnetic field reconnection as possible heating sources. We investigate here the viability of MHD-wave mediated cosmic ray heating as a supplemental heating source. This heating rate depends on the gas density only through its linear dependence on the Alfven speed, which goes as n{sub e}{sup -1/2}. We show that, scaled to appropriate values of cosmic ray energy density, cosmic ray heating can be significant. Furthermore, this heating is stable to perturbations. These results should also apply to warm ionized gas in other galaxies.

Wiener, Joshua; Peng Oh, S. [Department of Physics, University of California, Santa Barbara, CA 93106 (United States)] [Department of Physics, University of California, Santa Barbara, CA 93106 (United States); Zweibel, Ellen G. [Departments of Astronomy and Physics, and Center for Magnetic Self-Organization, University of Wisconsin-Madison, Madison, WI 53706 (United States)] [Departments of Astronomy and Physics, and Center for Magnetic Self-Organization, University of Wisconsin-Madison, Madison, WI 53706 (United States)

2013-04-10T23:59:59.000Z

447

Origin and propagation of the highest energy cosmic rays  

E-Print Network (OSTI)

In this lecture I give an overview of shock acceleration, interactions of high energy cosmic rays with, and propagation through, the background radiation, and the resulting electron-photon cascade. I argue that while the origin of the highest energy cosmic rays is still uncertain, it is not necessary to invoke exotic models such as emission by topological defects to explain the existing data. It seems likely that shock acceleration at Fanaroff-Riley Class II radio galaxies can account for the existing data. However, new cosmic ray data, as well as better estimates of the extragalactic radiation fields and magnetic fields will be necessary before we will be certain of the origin of the highest energy particles occurring in nature.

R. J. Protheroe

1996-12-22T23:59:59.000Z

448

Probing cosmic acceleration by using the SNLS3 SNIa dataset  

SciTech Connect

We probe the cosmic acceleration by using the recently released SNLS3 sample of 472 type Ia supernovae. Combining this type Ia supernovae dataset with the cosmic microwave background anisotropy data from the Wilkinson Microwave Anisotropy Probe 7-yr observations, the baryon acoustic oscillation results from the Sloan Digital Sky Survey data release 7, and the Hubble constant measurement from the Wide Field Camera 3 on the Hubble Space Telescope, we measure the dark energy equation of state w and the deceleration parameter q as functions of redshift by using the Chevallier-Polarski-Linder parametrization. Our result is consistent with a cosmological constant at 1? confidence level, without evidence for the recent slowing down of the cosmic acceleration. Furthermore, we consider three binned parametrizations (w is piecewise constant in redshift z) based on different binning methods. The similar results are obtained, i.e., the ?CDM model is still nicely compatible with current observations.

Li, Xiao-Dong; Wang, Shuang; Zhang, Wen-Shuai [Department of Modern Physics, University of Science and Technology of China, Hefei 230026 (China); Li, Song; Huang, Qing-Guo; Li, Miao, E-mail: renzhe@mail.ustc.edu.cn, E-mail: sli@itp.ac.cn, E-mail: swang@mail.ustc.edu.cn, E-mail: wszhang@mail.ustc.edu.cn, E-mail: huangqg@itp.ac.cn, E-mail: mli@itp.ac.cn [Institute of Theoretical Physics, Chinese Academy of Science, Beijing 100080 (China)

2011-07-01T23:59:59.000Z

449

Cosmic Ray Acceleration by Spiral Shocks in the Galactic Wind  

E-Print Network (OSTI)

Cosmic ray acceleration by shocks related with Slipping Interaction Regions (SIRs) in the Galactic Wind is considered. SIRs are similar to Solar Wind Corotating Interaction Regions. The spiral structure of our Galaxy results in a strong nonuniformity of the Galactic Wind flow and in SIR formation at distances of 50 to 100 kpc. SIRs are not corotating with the gas and magnetic field because the angular velocity of the spiral pattern differs from that of the Galactic rotation. It is shown that the collective reacceleration of the cosmic ray particles with charge $Ze$ in the resulting shock ensemble can explain the observable cosmic ray spectrum beyond the "knee" up to energies of the order of $10^{17}Z$ eV. For the reaccelerated particles the Galactic Wind termination shock acts as a reflecting boundary.

H. J. Voelk; V. N. Zirakashvili

2004-01-19T23:59:59.000Z

450

On the Nonlinear Evolution of Cosmic Web: Lagrangian Dynamics Revisited  

E-Print Network (OSTI)

We investigate the nonlinear evolution of cosmic morphologies of the large-scale structure by examining the Lagrangian dynamics of various tensors of a cosmic fluid element, including the velocity gradient tensor, the Hessian matrix of the gravitational potential as well as the deformation tensor. Instead of the eigenvalue representation, the first two tensors, which associate with the "kinematic" and "dynamical" cosmic web classification algorithm respectively, are studied in a more convenient parameter space. These parameters are defined as the rotational invariant coefficients of the characteristic equation of the tensor. In the nonlinear local model (NLM) where the magnetic part of Weyl tensor vanishes, these invariants are fully capable of characterizing the dynamics. Unlike the Zeldovich approximation (ZA), where various morphologies do not change before approaching a one-dimensional singularity, the sheets in NLM are unstable for both overdense and underdense perturbations. While it has long been known...

Wang, Xin

2014-01-01T23:59:59.000Z

451

Effects of inflation on a cosmic string loop population  

SciTech Connect

We study the evolution of simple cosmic string loop solutions in an inflationary universe. We show, for the particular case of circular loops, that periodic solutions do exist in a de Sitter universe, below a critical loop radius R{sub c}H=1/2. On the other hand, larger loops freeze in comoving coordinates, and we explicitly show that they can survive more e-foldings of inflation than pointlike objects. We discuss the implications of these findings for the survival of realistic cosmic string loops during inflation and for the general characteristics of post-inflationary cosmic string networks. We also consider the analogous solutions for domain walls, in which case the critical radius is R{sub c}H=2/3.

Avelino, P. P. [Centro de Fisica do Porto, Rua do Campo Alegre 687, 4169-007 Porto (Portugal); Departamento de Fisica da Faculdade de Ciencias da Universidade do Porto, Rua do Campo Alegre 687, 4169-007 Porto (Portugal); Martins, C. J. A. P. [Centro de Fisica do Porto, Rua do Campo Alegre 687, 4169-007 Porto (Portugal); Department of Applied Mathematics and Theoretical Physics, Centre for Mathematical Sciences, University of Cambridge, Wilberforce Road, Cambridge CB3 0WA (United Kingdom); Shellard, E. P. S. [Department of Applied Mathematics and Theoretical Physics, Centre for Mathematical Sciences, University of Cambridge, Wilberforce Road, Cambridge CB3 0WA (United Kingdom)

2007-10-15T23:59:59.000Z

452

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

453

Intense Muon Physics Working Group Summary  

E-Print Network (OSTI)

The intense muon beams which will be available at a neutrino factory provide a unique opportunity for searching for physics beyond the standard model, both in lepton flavor violation and in the search for a permanent electric dipole moment for the muon. Other experiments which can use intense muon beams will also be possible.

B. Lee Roberts; Marco Grassi; Akira Sato

2005-10-20T23:59:59.000Z

454

WINDS, CLUMPS, AND INTERACTING COSMIC RAYS IN M82  

SciTech Connect

We construct a family of models for the evolution of energetic particles in the starburst galaxy M82 and compare them to observations to test the calorimeter assumption that all cosmic ray energy is radiated in the starburst region. Assuming constant cosmic ray acceleration efficiency with Milky Way parameters, we calculate the cosmic-ray proton and primary and secondary electron/positron populations as a function of energy. Cosmic rays are injected with Galactic energy distributions and electron-to-proton ratio via Type II supernovae at the observed rate of 0.07 yr{sup -1}. From the cosmic ray spectra, we predict the radio synchrotron and {gamma}-ray spectra. To more accurately model the radio spectrum, we incorporate a multiphase interstellar medium in the starburst region of M82. Our model interstellar medium is highly fragmented with compact dense molecular clouds and dense photoionized gas, both embedded in a hot, low density medium in overall pressure equilibrium. The spectra predicted by this one-zone model are compared to the observed radio and {gamma}-ray spectra of M82. {chi}{sup 2} tests are used with radio and {gamma}-ray observations and a range of model predictions to find the best-fit parameters. The best-fit model yields constraints on key parameters in the starburst zone of M82, including a magnetic field strength of {approx}250 {mu}G and a wind advection speed in the range of 300-700 km s{sup -1}. We find that M82 is a good electron calorimeter but not an ideal cosmic-ray proton calorimeter and discuss the implications of our results for the astrophysics of the far-infrared-radio correlation in starburst galaxies.

Yoast-Hull, Tova M.; Everett, John E.; Zweibel, Ellen G. [Department of Physics, University of Wisconsin-Madison, WI (United States); Gallagher, J. S. III, E-mail: yoasthull@wisc.edu [Department of Astronomy, University of Wisconsin-Madison, WI (United States)

2013-05-01T23:59:59.000Z

455

Propagation of Cosmic Rays: Nuclear Physics in Cosmic-Ray Studies  

SciTech Connect

The nuclei fraction in cosmic rays (CR) far exceeds the fraction of other CR species, such as antiprotons, electrons, and positrons. Thus the majority of information obtained from CR studies is based on interpretation of isotopic abundances using CR propagation models where the nuclear data and isotopic production cross sections in p- and {alpha}-induced reactions are the key elements. This paper presents an introduction to the astrophysics of CR and diffuse {gamma}-rays and discusses some of the puzzles that have emerged recently due to more precise data and improved propagation models. Merging with cosmology and particle physics, astrophysics of CR has become a very dynamic field with a large potential of breakthrough and discoveries in the near future. Exploiting the data collected by the CR experiments to the fullest requires accurate nuclear cross sections.

Moskalenko, Igor V. [NASA/Goddard Space Flight Center, Code 661, Greenbelt, MD 20771 (United States); Joint Center for Astrophysics/University of Maryland, Baltimore County, Baltimore, MD 21250 (United States); Strong, Andrew W. [Max-Planck-Institut fuer extraterrestrische Physik, Postfach 1603, D-85740 Garching (Germany); Mashnik, Stepan G. [Los Alamos National Laboratory, Los Alamos, NM 87544 (United States)

2005-05-24T23:59:59.000Z

456

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

457

Description of Energy Intensity Tables (12)  

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

3. Description of Energy Intensity Data Tables 3. Description of Energy Intensity Data Tables There are 12 data tables used as references for this report. Specifically, these tables are categorized as tables 1 and 2 present unadjusted energy-intensity ratios for Offsite-Produced Energy and Total Inputs of Energy for 1985, 1988, 1991, and 1994; along with the percentage changes between 1985 and the three subsequent years (1988, 1991, and 1994) tables 3 and 4 present 1988, 1991, and 1994 energy-intensity ratios that have been adjusted to the mix of products shipped from manufacturing establishments in 1985 tables 5 and 6 present unadjusted energy-intensity ratios for Offsite-Produced Energy and Total Inputs of Energy for 1988, 1991, and 1994; along with the percentage changes between 1988 and the two subsequent

458

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

459

High energy cosmic rays, gamma rays and neutrinos from AGN  

E-Print Network (OSTI)

The author reviews a model for the emission of high energy cosmic rays, gamma-rays and neutrinos from AGN (Active Galactic Nuclei) that he has proposed since 1985. Further discussion of the knee energy phenomenon of the cosmic ray energy spectrum requires the existence of a heavy particle with mass in the knee energy range. A possible method of detecting such a particle in the Pierre Auger Project is suggested. Also presented is a relation between the spectra of neutrinos and gamma-rays emitted from AGN. This relation can be tested by high energy neutrino detectors such as ICECUBE, the Mediterranean Sea Detector and possibly by the Pierre Auger Project.

Yukio Tomozawa

2008-02-03T23:59:59.000Z

460

Cosmic ray abundance measurements with the CAKE balloon experiment  

E-Print Network (OSTI)

We present the results from the CAKE (Cosmic Abundance below Knee Energy) balloon experiment which uses nuclear track detectors. The final experiment goal is the determination of the charge spectrum of CR nuclei with Z > 30 in the primary cosmic radiation. The detector, which has a geometric acceptance of \\~ 1.7 m2 sr, was exposed in a trans-mediterranean stratospheric balloon flight. Calibrations of the detectors used (CR39 and Lexan), scanning strategies and algorithms for tracking particles in an automatic mode are presented. The present status of the results is discussed

S. Cecchini; T. Chiarusi; G. Giacomelli; S. Manzoor; E. Medinaceli; L. Patrizii; V. Togo

2005-10-25T23:59:59.000Z

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.


461

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

462

Large scale EPR correlations and cosmic gravitational waves  

E-Print Network (OSTI)

We study how quantum correlations survive at large scales in spite of their exposition to stochastic backgrounds of gravitational waves. We consider Einstein-Podolski-Rosen (EPR) correlations built up on the polarizations of photon pairs and evaluate how they are affected by the cosmic gravitational wave background (CGWB). We evaluate the quantum decoherence of the EPR correlations in terms of a reduction of the violation of the Bell inequality as written by Clauser, Horne, Shimony and Holt (CHSH). We show that this decoherence remains small and that EPR correlations can in principle survive up to the largest cosmic scales.

B. Lamine; R. Herv; M. -T. Jaekel; A. Lambrecht; S. Reynaud

2011-05-10T23:59:59.000Z

463

RADIOGRAPHIC IMAGING BELOW A VOLCANIC CRATER FLOOR WITH COSMIC-RAY MUONS  

E-Print Network (OSTI)

horizontally-arriving cosmic ray muon with energy of 1 TeV can penetrate 2.6 km of water. Thus, cosmic-ray muon that uncertainty on the shape and amplitude of the energy spectrum of the muon source is within a few percentRADIOGRAPHIC IMAGING BELOW A VOLCANIC CRATER FLOOR WITH COSMIC-RAY MUONS HIROYUKI K.M. TANAKA

Aoki, Yosuke

464

Impact Factors of Energy Intensity in China  

E-Print Network (OSTI)

Energy intensity reflects energy usage efficiency in the production and consumption process, and leads to carbon dioxide emissions and the energy security of an economy. Liao et al. (2007) analyzed factors contribute to the fluctuation of Chinas energy intensity from 1997 to 2006, and found that efficiency effects and structural effects are the major impacting factors. Therefore, they suggested that China should attach more importance to optimizing its sectoral structure, and lowering its investment ratio in the future. However, economic development and energy intensity are influenced by many factors. In their research, Liao et al. (2007) omitted some important contributing factors to energy intensities, and their suggestions also had some practical limitations. First of all, Liao et al. (2007) did not analyze impacts from energy prices in energy usage efficiency. In the existing literature, Birol and Keppler (2000) applied economics theory and suggested that higher energy prices can induce the improvements in energy usage efficiency, thereby lowering energy intensity. Hang and Tu (2007) studied the influence of energy price on the Chinese economy's energy intensity and their empirical results also showed that higher energy prices can lower energy intensity. Because energy prices have been regulated by the

unknown authors

465

Heavy Quark and Neutrino Physics Final Report 2011 2014  

SciTech Connect

This final closeout report covers research supported by the ``Heavy Quark and Neutrino Physics'' grant at Kansas State University during the grant's last renewal period, November 1, 2011, through April 30, 2014. The report begins with an overview of the group, its goals and activities, and personnel. Then summaries are given of achievements in each of the three frontiers: Energy Frontier research in the D0 and CMS experiments; Intensity Frontier research in the Double Chooz and ArgoNeuT experiments as well as research and development for MicroBooNE and LBNE; and Cosmic Frontier and Theoretical research. The report concludes with a list of publications supported by this grant in which our group made a significant contribution during the reporting period, followed by a list of students partially or fully supported by the grant who were awarded a PhD during this period.

Horton-Smith, Glenn A. [Kansas State University] (ORCID:0000000196779167); Bolton, Timothy [Kansas State University; Ivanov, Andrew [Kansas State University; Maravin, Yurii [Kansas State University; Ratra, Bharat [Kansas State University

2014-07-21T23:59:59.000Z

466

Techniques for optically compressing light intensity ranges  

DOE Patents (OSTI)

A pin hole camera assembly for use in viewing an object having a relatively large light intensity range, for example a crucible containing molten uranium in an atomic vapor laser isotope separator (AVLIS) system is disclosed herein. The assembly includes means for optically compressing the light intensity range appearing at its input sufficient to make it receivable and decipherable by a standard video camera. A number of different means for compressing the intensity range are disclosed. These include the use of photogray glass, the use of a pair of interference filters, and the utilization of a new liquid crystal notch filter in combination with an interference filter.

Rushford, Michael C. (Livermore, CA)

1989-01-01T23:59:59.000Z

467

Techniques for optically compressing light intensity ranges  

DOE Patents (OSTI)

A pin hole camera assembly for use in viewing an object having a relatively large light intensity range, for example a crucible containing molten uranium in an atomic vapor laser isotope separator (AVLIS) system is disclosed herein. The assembly includes means for optically compressing the light intensity range appearing at its input sufficient to make it receivable and decipherable by a standard video camera. A number of different means for compressing the intensity range are disclosed. These include the use of photogray glass, the use of a pair of interference filters, and the utilization of a new liquid crystal notch filter in combination with an interference filter. 18 figs.

Rushford, M.C.

1989-03-28T23:59:59.000Z

468

EXPLAIN COSMIC ACCELERATION? FIRST, CORRECT EINSTEIN HOMER G. ELLIS  

E-Print Network (OSTI)

. Keywords: Cosmic acceleration; dark matter/energy; in ation. Cosmologists are perplexed by the discovery matter into galaxies and galactic clusters and superclusters, an even more mysterious `dark energy this dark energy by Einstein's cosmological constant #3;, attributing its source to a negative pressure

Ellis, Homer

469

A model for the cosmic creation of nuclear exergy  

Science Journals Connector (OSTI)

... Although the problem of cosmic exergy creation has not been widely discussed, general answers have been given by Tolman3, and ... can be extracted from a system only to the extent that this deviates from equilibrium. Exergy is thus a measure of deviation from equilibrium, of contrast, internally or against an ...

K.-E. Eriksson, S. Islam, B.-S. Skagerstam

1982-04-08T23:59:59.000Z

470

EMMA an underground cosmic-ray experiment T. Enqvista  

E-Print Network (OSTI)

distribution function of high-energy muons. The rock overbur- den filters out all other charged particles of the air shower except the high-energy muons. The over- burden of 75 metres (corresponding to 210 m of cosmic rays at and above the knee region. The array, called EMMA (Experiment with MultiMuon Array

Usoskin, Ilya G.

471

Energy spectrum of cosmic-ray muons at sea level  

Science Journals Connector (OSTI)

The integral energy spectrum of cosmic-ray muons at sea level in the energy range (2007500) GeV is deduced ... this, the effect of fluctuations in the energy losses of muons is taken into account. The deduced muon

S. Miyake; V. S. Narasimham; P. V. Ramana Murthy

1964-01-16T23:59:59.000Z

472

Macroscopic quantum tunneling and the 'cosmic' Josephson effect  

SciTech Connect

We discuss the possible influence of a cosmic magnetic field on the macroscopic quantum tunneling process associated, in a cosmological context, to the decay of the 'false vacuum'. We find a close analogy with the effects of an external magnetic field applied to a Josephson junction in the context of low-temperature/high-temperature superconducting devices.

Barone, A. [Dipartimento di Scienze Fisiche, Universita di Napoli 'Federico II', CNR-SPIN, Piazzale Tecchio 21, 80125 Napoli (Italy); Gasperini, M. [Dipartimento di Fisica, Universita di Bari, Via G. Amendola 173, 70126 Bari (Italy); INFN, Sezione di Bari, Bari (Italy); Rotoli, G. [Dipartimento di Ingegneria dell'Informazione, Seconda Universita di Napoli (SUN), Via Roma 29, 81031 Aversa (CE) (Italy)

2010-10-15T23:59:59.000Z

473

Cosmic rays, lithium abundance and excess entropy in galaxy clusters  

E-Print Network (OSTI)

We consider the production of $^6$Li in spallation reactions by cosmic rays in order to explain the observed abundance in halo metal-poor stars. We show that heating of ambient gas by cosmic rays is an inevitable consequence of this process, and estimate the energy input required to reproduce the observed abundance of $^6$Li/H$\\sim 10^{-11}$ to be of order a few hundred eV per particle. We draw attention to the possibility that this could explain the excess entropy in gas in galaxy groups and clusters. The evolution of $^6$Li and the accompanying heating of gas is calculated for structures collapsing at the present epoch with injection of cosmic rays at high redshift. We determine the energy required to explain the abundance of $^6$Li at $z \\sim 2$ corresponding to the formation epoch of halo metal-poor stars, and also an increased entropy level of $\\sim 300$ keV cm$^2$ necessary to explain X-ray observations of clusters. The energy budget for this process is consistent with the expected energy output of radio-loud AGNs, and the diffusion length scale of cosmic-ray protons responsible for heating is comparable to the size of regions with excess entropy. We also discuss the constraints imposed by the extragalactic gamma-ray background.

Biman B. Nath; Piero Madau; Joseph Silk

2005-11-21T23:59:59.000Z

474

Concerning the Nature of the Cosmic Ray Power Law Exponents  

E-Print Network (OSTI)

We have recently shown that the cosmic ray energy distributions as detected on earthbound, low flying balloon or high flying satellite detectors can be computed by employing the heats of evaporation of high energy particles from astrophysical sources. In this manner, the experimentally well known power law exponents of the cosmic ray energy distribution have been theoretically computed as 2.701178 for the case of ideal Bose statistics, 3.000000 for the case of ideal Boltzmann statistics and 3.151374 for the case of ideal Fermi statistics. By "ideal" we mean virtually zero mass (i.e. ultra-relativistic) and noninteracting. These results are in excellent agreement with the experimental indices of 2.7 with a shift to 3.1 at the high energy ~ PeV "knee" in the energy distribution. Our purpose here is to discuss the nature of cosmic ray power law exponents obtained by employing conventional thermal quantum field theoretical models such as quantum chromodynamics to the cosmic ray sources in a thermodynamic scheme wherein gamma and zeta function regulation is employed. The key reason for the surprising accuracy of the ideal boson and ideal fermion cases resides in the asymptotic freedom or equivalently the Feynman "parton" structure of the ultra-high energy tails of spectral functions.

A. Widom; J. Swain; Y. N. Srivastava

2014-10-15T23:59:59.000Z

475

Cosmic Ray Pitch Angle Scattering Through 90 o  

E-Print Network (OSTI)

Cosmic Ray Pitch Angle Scattering Through 90 o G.M. Felice 1 and R.M. Kulsrud 2 Princeton Plasma­ lar attention to the problem of particle scattering through the # = cos -1 (v # /v) = 90 o pitch angle their pitch angle by mirror interaction with long wavelength waves generated by the # # 0 particles. We match

476

Concerning the Nature of the Cosmic Ray Power Law Exponents  

E-Print Network (OSTI)

We have recently shown that the cosmic ray energy distributions as detected on earthbound, low flying balloon or high flying satellite detectors can be computed by employing the heats of evaporation of high energy particles from astrophysical sources. In this manner, the experimentally well known power law exponents of the cosmic ray energy distribution have been theoretically computed as 2.701178 for the case of ideal Bose statistics, 3.000000 for the case of ideal Boltzmann statistics and 3.151374 for the case of ideal Fermi statistics. By "ideal" we mean virtually zero mass (i.e. ultra-relativistic) and noninteracting. These results are in excellent agreement with the experimental indices of 2.7 with a shift to 3.1 at the high energy ~ PeV "knee" in the energy distribution. Our purpose here is to discuss the nature of cosmic ray power law exponents obtained by employing conventional thermal quantum field theoretical models such as quantum chromodynamics to the cosmic ray sources in a thermodynamic scheme w...

Widom, A; Srivastava, Y N

2014-01-01T23:59:59.000Z

477

Ultra-high energy cosmic rays from Quark Novae  

E-Print Network (OSTI)

We explore acceleration of ions in the Quark Nova (QN) scenario, where a neutron star experiences an explosive phase transition into a quark star (born in the propeller regime). In this picture, two cosmic ray components are isolated: one related to the randomized pulsar wind and the other to the propelled wind, both boosted by the ultra-relativistic Quark Nova shock. The latter component acquires energies $10^{15} {\\rm eV}wind, achieves ultra-high energies $E> 10^{18.6}$ eV. The composition is dominated by ions present in the pulsar wind in the energy range above $10^{18.6}$ eV, while at energies below $10^{18}$ eV the propelled ejecta, consisting of the fall-back neutron star crust material from the explosion, is the dominant one. Added to these two components, the propeller injects relativistic particles with Lorentz factors $\\Gamma_{\\rm prop.} \\sim 1-1000$, later to be accelerated by galactic supernova shocks. The QN model appears to be able to account for the extragalactic cosmic rays above the ankle and to contribute a few percent of the galactic cosmic rays below the ankle. We predict few hundred ultra-high energy cosmic ray events above $10^{19}$ eV for the Pierre Auger detector per distant QN, while some thousands are predicted for the proposed EUSO and OWL detectors.

R. Ouyed; P. Kernen; J. Maalampi

2003-01-29T23:59:59.000Z

478

Cosmic Hide and Seek: Tracking Missing and Invisible  

E-Print Network (OSTI)

Cosmic Hide and Seek: Tracking Missing and Invisible Matter in the Universe Sheila Kannappan-Forming Cloud NASA/Spitzer #12;...or in the radio? the invisible becomes visible · stars are bright at optical-bending socks ­ have to exist, but invisible at any wavelength #12;Lost Sock Classification · black & blue socks

Kannappan, Sheila

479

Signature of cosmic string wakes in the CMB polarization  

SciTech Connect

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

480

Building dependability arguments for software intensive systems  

E-Print Network (OSTI)

A method is introduced for structuring and guiding the development of end-to-end dependability arguments. The goal is to establish high-level requirements of complex software-intensive systems, especially properties that ...

Seater, Robert Morrison

2009-01-01T23:59:59.000Z

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.


481

Computational phase imaging based on intensity transport  

E-Print Network (OSTI)

Light is a wave, having both an amplitude and a phase. However, optical frequencies are too high to allow direct detection of phase; thus, our eyes and cameras see only real values - intensity. Phase carries important ...

Waller, Laura A. (Laura Ann)

2010-01-01T23:59:59.000Z

482

Modelling patient states in intensive care patients  

E-Print Network (OSTI)

Extensive bedside monitoring in hospital Intensive Care Units (ICU) has resulted in a deluge of information on patient physiology. Consequently, clinical decision makers have to reason with data that is simultaneously large ...

Kshetri, Kanak Bikram

2011-01-01T23:59:59.000Z

483

Transport of elliptic intense charged -particle beams  

E-Print Network (OSTI)

The transport theory of high-intensity elliptic charged-particle beams is presented. In particular, the halo formation and beam loss problem associated with the high space charge and small-aperture structure is addressed, ...

Zhou, J. (Jing), 1978-

2006-01-01T23:59:59.000Z

484

Technical Change, Investment and Energy Intensity  

E-Print Network (OSTI)

This paper analyzes the role of different components of technical change on energy intensity by applying a Translog variable cost function setting to the new EU KLEMS dataset for 3 selected EU countries (Italy, Finland and ...

Kratena, Kurt

485

Sustaining Performance Improvements in Energy Intensive Industries  

E-Print Network (OSTI)

Experience has shown that significant opportunity for performance improvements exists in energy intensive operations. Often, efforts to improve efficiency focus on vendor-led initiatives to improve operations of particular equipment. This approach...

Moore, D. A.

2005-01-01T23:59:59.000Z

486

Absolute vs. intensity-based emission caps  

E-Print Network (OSTI)

Cap-and-trade systems limit emissions to some pre-specified absolute quantity. Intensity-based limits, that restrict emissions to some pre-specified rate relative to input or output, are much more widely used in environmental ...

Ellerman, A. Denny.

487

Laser intensity effects in noncommutative QED  

E-Print Network (OSTI)

We discuss a two-fold extension of QED assuming the presence of strong external fields provided by an ultra-intense laser and noncommutativity of spacetime. While noncommutative effects leave the electron's intensity induced mass shift unchanged, the photons change significantly in character: they acquire a quasi-momentum that is no longer light-like. We study the consequences of this combined noncommutative strong-field effect for basic lepton-photon interactions.

Thomas Heinzl; Anton Ilderton; Mattias Marklund

2010-02-17T23:59:59.000Z

488

The 2dF Galaxy Redshift Survey: constraints on cosmic star-formation history from the cosmic spectrum  

E-Print Network (OSTI)

We present the first results on the history of star formation in the Universe based on the `cosmic spectrum', in particular, the volume-averaged, luminosity-weighted, stellar absorption line spectrum of present day galaxies from the 2dFGRS. This method is novel in that unlike previous studies it is not an estimator based on total luminosity density. The cosmic spectrum is fitted with models of population synthesis, tracing the history of star formation prior to the epoch of the observed galaxies, using a method we have developed which decouples continuum and spectral-line variations and is robust against spectrophotometric uncertainties. The cosmic spectrum can only be fitted with models incorporating chemical evolution and indicates there was a peak of star-formation rate in the past of at least three times the current value and that the increase back to z=1, assuming it scales as (1+z)^beta, has a strong upper limit of beta1: e.g., if beta>2 then the SFR for 11. Our results are consistent with the best-fit results from compilations of cosmic SFR estimates based on UV luminosity density, which give 1.8

I. K. Baldry; K. Glazebrook; C. M. Baugh; J. Bland-Hawthorn; T. Bridges; R. Cannon; S. Cole; M. Colless; C. Collins; W. Couch; G. Dalton; R. De Propris; S. P. Driver; G. Efstathiou; R. S. Ellis; C. S. Frenk; E. Hawkins; C. Jackson; O. Lahav; I. Lewis; S. Lumsden; S. Maddox; D. S. Madgwick; P. Norberg; J. A. Peacock; B. A. Peterson; W. Sutherland; K. Taylor

2002-01-03T23:59:59.000Z

489

ON COMPUTING UPPER LIMITS TO SOURCE INTENSITIES  

SciTech Connect

A common problem in astrophysics is determining how bright a source could be and still not be detected in an observation. Despite the simplicity with which the problem can be stated, the solution involves complicated statistical issues that require careful analysis. In contrast to the more familiar confidence bound, this concept has never been formally analyzed, leading to a great variety of often ad hoc solutions. Here we formulate and describe the problem in a self-consistent manner. Detection significance is usually defined by the acceptable proportion of false positives (background fluctuations that are claimed as detections, or Type I error), and we invoke the complementary concept of false negatives (real sources that go undetected, or Type II error), based on the statistical power of a test, to compute an upper limit to the detectable source intensity. To determine the minimum intensity that a source must have for it to be detected, we first define a detection threshold and then compute the probabilities of detecting sources of various intensities at the given threshold. The intensity that corresponds to the specified Type II error probability defines that minimum intensity and is identified as the upper limit. Thus, an upper limit is a characteristic of the detection procedure rather than the strength of any particular source. It should not be confused with confidence intervals or other estimates of source intensity. This is particularly important given the large number of catalogs that are being generated from increasingly sensitive surveys. We discuss, with examples, the differences between these upper limits and confidence bounds. Both measures are useful quantities that should be reported in order to extract the most science from catalogs, though they answer different statistical questions: an upper bound describes an inference range on the source intensity, while an upper limit calibrates the detection process. We provide a recipe for computing upper limits that applies to all detection algorithms.

Kashyap, Vinay L.; Siemiginowska, Aneta [Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138 (United States); Van Dyk, David A.; Xu Jin [Department of Statistics, University of California, Irvine, CA 92697-1250 (United States); Connors, Alanna [Eureka Scientific, 2452 Delmer Street, Suite 100, Oakland, CA 94602-3017 (United States); Freeman, Peter E. [Department of Statistics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213 (United States); Zezas, Andreas, E-mail: vkashyap@cfa.harvard.ed, E-mail: asiemiginowska@cfa.harvard.ed, E-mail: dvd@ics.uci.ed, E-mail: jinx@ics.uci.ed, E-mail: aconnors@eurekabayes.co, E-mail: pfreeman@cmu.ed, E-mail: azezas@cfa.harvard.ed [Physics Department, University of Crete, P.O. Box 2208, GR-710 03, Heraklion, Crete (Greece)

2010-08-10T23:59:59.000Z

490

Mould incidence and mycotoxin contamination in maize kernels from Swat Valley, North West Frontier Province of Pakistan  

Science Journals Connector (OSTI)

Mould incidence and aflatoxin B1 (AFB1) and ochratoxin A (OTA) contamination as well as proximate composition and minerals content of maize kernels from Swat Valley, North West Frontier Province of Pakistan was studied during the year, 2007. Results indicated that the mean moisture content of the kernels was within the recommended safe storage levels of ?15%. Across the whole valley, Aspergillus, Fusarium, Penicillium and Rhizopus were the most predominant fungal genera identified and amongst the mycotoxigenic species, Aspergillus flavus had the highest incidence. AFB1 content ranged from none to 30.92?g/kg with the average values of 14.94 and 16.22?g/kg for Upper and Lower Swat regions, respectively. Similar trend was observed for OTA with the contamination level ranged from Valley may be exposed to the danger of aflatoxins and ochratoxins poisoning. Thus, there is a need for policy makers to establish and enforce maize quality standards and regulations related to moulds and mycotoxins across the area.

Hamid Ullah Shah; Thomas J. Simpson; Sahib Alam; Khanzadi Fatima Khattak; Sajida Perveen

2010-01-01T23:59:59.000Z

491

Energy Frontier Research Centers: Helping Win the Energy Innovation Race (2011 EFRC Summit Keynote Address, Secretary of Energy Chu)  

ScienceCinema (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)

2012-03-14T23:59:59.000Z

492

MUSE integral-field spectroscopy towards the Frontier Fields Cluster Abell S1063: I. Data products and redshift identifications  

E-Print Network (OSTI)

We present the first observations of the Frontier Fields Cluster Abell S1063, taken with the newly commissioned Multi Unit Spectroscopic Explorer (MUSE) integral field spectrograph. Because of the relatively large field of view (1 arcmin^2), MUSE is ideal to simultaneously target multiple galaxies in blank and cluster fields over the full optical spectrum. We analysed the four hours of data obtained in the Science Verification phase on this cluster and measured redshifts for 60 objects. We confirm the redshift of five cluster galaxies, and determine the redshift of 28 other cluster members. Behind the cluster, we find 16 galaxies at higher redshift, including three previously unknown Lyman-alpha emitters at z>3, and five multiply-lensed galaxies. We report the detection of a new z=4.113 multiply lensed galaxy, with images that are consistent with lensing model predictions derived for the Fronter Fields. We detect CIII], C IV and He II emission in a multiply lensed galaxy at z=3.116, suggesting the likely pres...

Karman, W; Grillo, C; Balestra, I; Rosati, P; Vanzella, E; Coe, D; Christensen, L; Koekemoer, A M; Kruehler, T; Lombardi, M; Mercurio, A; Nonino, M; van der Wel, A

2014-01-01T23:59:59.000Z

493

A Rigorous Free-form Lens Model of Abell 2744 to Meet the Hubble Frontier Fields Challenge  

E-Print Network (OSTI)

Deep Hubble Frontier Fields (HFF) imaging of the most powerful lensing clusters provides access to the most magnified distant galaxies. It is a challenge to construct lens models capable of describing these complex massive, merging clusters so that the intrinsic source properties can be meaningfully derived. Here we apply our general free-form lensing method (WSLAP+) to A2744, providing a model independent map of the cluster magnification and geometric distance estimates to multiply-lensed sources. We solve simultaneously for a smooth cluster component on a pixel grid, together with local deflections by the observed member galaxies. Our solution is sufficiently accurate to securely identify 18 multiply-lensed systems behind A2744 totaling 56 images, spanning 1.0

Lam, Daniel; Diego, Jose M; Lim, Jeremy; Coe, Dan; Ford, Holland C; Zheng, Wei

2014-01-01T23:59:59.000Z

494

Future High-Intensity Proton Accelerators  

E-Print Network (OSTI)

This paper provides an overview of currently planned high-intensity proton accelerators. While for high energies (>10GeV) synchrotrons remain the preferred tools to produce high-intensity beams, recent years have seen an impressive development of linac-based lower-energy (intensity proton drivers for spallation sources, accelerator driven systems (ADS), production of Radioactive Ion Beams (RIB) and various neutrino applications (beta-beam, superbeam, neutrino factory). This paper discusses the optimum machine types for the various beam requirements and uses a range of projects, which are likely to be realised within the coming decade, to illustrate the different approaches to reach high average beam power with the application-specific time structure. Only machines with a beam power above 100kW are considered.

Gerigk, F

2007-01-01T23:59:59.000Z

495

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

496

Testing gaussianity, homogeneity and isotropy with the cosmic microwave background  

E-Print Network (OSTI)

We review the basic hypotheses which motivate the statistical framework used to analyze the cosmic microwave background, and how that framework can be enlarged as we relax those hypotheses. In particular, we try to separate as much as possible the questions of gaussianity, homogeneity and isotropy from each other. We focus both on isotropic estimators of non-gaussianity as well as statistically anisotropic estimators of gaussianity, giving particular emphasis on their signatures and the enhanced "cosmic variances" that become increasingly important as our putative Universe becomes less symmetric. After reviewing the formalism behind some simple model-independent tests, we discuss how these tests can be applied to CMB data when searching for large scale "anomalies"

L. Raul Abramo; Thiago S. Pereira

2010-05-13T23:59:59.000Z

497

Extended Mosaic Observations with the Cosmic Background Imager  

E-Print Network (OSTI)

Two years of microwave background observations with the Cosmic Background Imager (CBI) have been combined to give a sensitive, high resolution angular power spectrum over the range 400 2000 power previously seen with the CBI is reduced. Under the assumption that any signal in excess of the primary anisotropy is due to a secondary Sunyaev-Zeldovich anisotropy in distant galaxy clusters we use CBI, ACBAR, and BIMA data to place a constraint on the present-day rms mass fluctuation sigma_8. We present the results of a cosmological parameter analysis on the l < 2000 primary anisotropy data which show significant improvements in the parameters as compared to WMAP alone, and we explore the role of the small-scale cosmic microwave background data in breaking parameter degeneracies.

A. C. S. Readhead; B. S. Mason; C. R. Contaldi; T. J. Pearson; J. R. Bond; S. T. Myers; S. Padin; J. L. Sievers; J. K. Cartwright; M. C. Shepherd; D. Pogosyan; S. Prunet; P. Altamirano; R. Bustos; L. Bronfman; S. Casassus; W. L. Holzapfel; J. May; U. -L. Pen; S. Torres; P. S. Udomprasert

2004-02-15T23:59:59.000Z

498

Ankle phenomenon in the cosmic ray energy spectrum  

E-Print Network (OSTI)

The author has suggested that the knee phenomenon in the cosmic ray energy spectrum at 3 PeV can be explained as a split between a radiation-dominated expansion and a matter-dominated expansion of an expanding heat bath. The model proposed in 1985, in fact, predicted that high energy cosmic rays are emitted from AGN, massive black holes, in agreement with recent data from the Pierre Auger Observatory. Similarly, the ankle phenomenon at 3 EeV is shown to be explained by a split between inflational expansion and ordinary material expansion of the expanding heat bath, not unlike that in the expansion of the universe. All the spectral indicies in the respective regions of the energy spectra agree with the theoretical calculation from the respective expansion rates.

Yukio Tomozawa

2012-08-22T23:59:59.000Z

499

Ankle phenomenon in the cosmic ray energy spectrum  

E-Print Network (OSTI)

The author has suggested that the knee phenomenon in the cosmic ray energy spectrum at 3 PeV can be explained as a split between a radiation-dominated expansion and a matter-dominated expansion of an expanding heat bath. The model proposed in 1985, in fact, predicted that high energy cosmic rays are emitted from AGN, massive black holes, in agreement with recent data from the Pierre Auger Observatory. Similarly, the ankle phenomenon at 3 EeV is shown to be explained by a split between inflational expansion and ordinary material expansion of the expanding heat bath, not unlike that in the expansion of the universe. All the spectral indicies in the respective regions of the energy spectra agree with the theoretical calculation from the respective expansion rates.

Tomozawa, Yukio

2012-01-01T23:59:59.000Z

500

Fundamental constants and cosmic vacuum: the micro and macro connection  

E-Print Network (OSTI)

The idea that the vacuum energy density $\\rho_{\\Lambda}$ could be time dependent is a most reasonable one in the expanding Universe; in fact, much more reasonable than just a rigid cosmological constant for the entire cosmic history. Being $\\rho_{\\Lambda}=\\rho_{\\Lambda}(t)$ dynamical, it offers a possibility to tackle the cosmological constant problem in its various facets. Furthermore, for a long time (most prominently since Dirac's first proposal on a time variable gravitational coupling) the possibility that the fundamental "constants" of Nature are slowly drifting with the cosmic expansion has been continuously investigated. In the last two decades, and specially in recent times, mounting experimental evidence attests that this could be the case. In this paper, we consider the possibility that these two groups of facts might be intimately connected, namely that the observed acceleration of the Universe and the possible time variation of the fundamental constants are two manifestations of the same underlyi...

Fritzsch, Harald

2015-01-01T23:59:59.000Z