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1

Construction Kathryn Hess  

E-Print Network [OSTI]

The Cobar Construction Kathryn Hess A (neo)classical approach Topological applications of DCSH structure On beyond chain complexes The Cobar Construction Kathryn Hess Institute of Geometry, Algebra 2006 #12;The Cobar Construction Kathryn Hess A (neo)classical approach Topological applications of DCSH

Thévenaz, Jacques

2

Nancy J. Hess | EMSL  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsrucLas Conchas recoveryLaboratory | NationalJohn F. Geisz,AerialStaff NUG 2012NakayasuJ. Hess Recent

3

38017,"AMERADA HESS CORP ",1,130,"MOTOR...  

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

SUPPLY CO ",55,850,"UNFINISHED OILS, RESIDUUM",5312,"CORPUS CHRIS, TX","TEXAS",3,428,"GERMANY",543,0,0,"VALERO REFG CO ","CORPUS CHRISTI","TX","TEXAS",3 38017,"VALERO MKTG &...

4

Systems of Hess-Appel'rot type  

E-Print Network [OSTI]

We construct higher-dimensional generalizations of the classical Hess-Appel'rot rigid body system. We give a Lax pair with a spectral parameter leading to an algebro-geometric integration of this new class of systems, which is closely related to the integration of the Lagrange bitop performed by us recently and uses Mumford relation for theta divisors of double unramified coverings. Based on the basic properties satisfied by such a class of systems related to bi-Poisson structure, quasi-homogeneity, and conditions on the Kowalevski exponents, we suggest an axiomatic approach leading to what we call the "class of systems of Hess-Appel'rot type".

Vladimir Dragovic; Borislav Gajic

2006-02-09T23:59:59.000Z

5

Hydrology and Earth System Sciences, 10, 3148, 2006 www.copernicus.org/EGU/hess/hess/10/31/  

E-Print Network [OSTI]

Hydrology and Earth System Sciences, 10, 31­48, 2006 www.copernicus.org/EGU/hess/hess/10/31/ SRef-ID: 1607-7938/hess/2006-10-31 European Geosciences Union Hydrology and Earth System Sciences Transport International Centre for Hydrology "Dino Tonini" and Dipartimento IMAGE, Universit`a di Padova, via Loredan 20

Paris-Sud XI, Université de

6

Hydrology and Earth System Sciences, 9, 111126, 2005 www.copernicus.org/EGU/hess/hess/9/111/  

E-Print Network [OSTI]

Hydrology and Earth System Sciences, 9, 111­126, 2005 www.copernicus.org/EGU/hess/hess/9/111/ SRef-ID: 1607-7938/hess/2005-9-111 European Geosciences Union Hydrology and Earth System Sciences Constraints of artificial neural networks for rainfall-runoff modelling: trade-offs in hydrological state representation

Paris-Sud XI, Université de

7

Hydrology and Earth System Sciences, 10, 1929, 2006 www.copernicus.org/EGU/hess/hess/10/19/  

E-Print Network [OSTI]

Hydrology and Earth System Sciences, 10, 19­29, 2006 www.copernicus.org/EGU/hess/hess/10/19/ SRef-ID: 1607-7938/hess/2006-10-19 European Geosciences Union Hydrology and Earth System Sciences Transport. Marani International Centre for Hydrology "Dino Tonini" and Dipartimento IMAGE, Universit`a di Padova

Boyer, Edmond

8

Hydrology and Earth System Sciences, 10, 127137, 2006 www.copernicus.org/EGU/hess/hess/10/127/  

E-Print Network [OSTI]

Hydrology and Earth System Sciences, 10, 127­137, 2006 www.copernicus.org/EGU/hess/hess/10/127/ SRef-ID: 1607-7938/hess/2006-10-127 European Geosciences Union Hydrology and Earth System Sciences Centre, Maun, Botswana Received: 11 August 2005 ­ Published in Hydrology and Earth System Sciences

Paris-Sud XI, Université de

9

Hydrology and Earth System Sciences, 9, 314, 2005 www.copernicus.org/EGU/hess/hess/9/3/  

E-Print Network [OSTI]

Hydrology and Earth System Sciences, 9, 3­14, 2005 www.copernicus.org/EGU/hess/hess/9/3/ SRef-ID: 1607-7938/hess/2005-9-3 European Geosciences Union Hydrology and Earth System Sciences Bringing it all, Dublin, Ireland Received: 6 December 2004 ­ Published in Hydrology and Earth System Sciences Discussions

Paris-Sud XI, Université de

10

Hydrology and Earth System Sciences, 9, 139155, 2005 www.copernicus.org/EGU/hess/hess/9/139/  

E-Print Network [OSTI]

Hydrology and Earth System Sciences, 9, 139­155, 2005 www.copernicus.org/EGU/hess/hess/9/139/ SRef-ID: 1607-7938/hess/2005-9-139 European Geosciences Union Hydrology and Earth System Sciences Using stable isotope tracers to assess hydrological flow paths, residence times and landscape influences in a nested

Paris-Sud XI, Université de

11

Hydrology and Earth System Sciences, 9, 173183, 2005 www.copernicus.org/EGU/hess/hess/9/173/  

E-Print Network [OSTI]

Hydrology and Earth System Sciences, 9, 173­183, 2005 www.copernicus.org/EGU/hess/hess/9/173/ SRef-ID: 1607-7938/hess/2005-9-173 European Geosciences Union Hydrology and Earth System Sciences Soil moisture ­ Published in Hydrology and Earth System Sciences Discussions: 2 March 2005 Revised: 29 June 2005 ­ Accepted

Paris-Sud XI, Université de

12

Hydrology and Earth System Sciences, 10, 7991, 2006 www.copernicus.org/EGU/hess/hess/10/79/  

E-Print Network [OSTI]

Hydrology and Earth System Sciences, 10, 79­91, 2006 www.copernicus.org/EGU/hess/hess/10/79/ SRef-ID: 1607-7938/hess/2006-10-79 European Geosciences Union Hydrology and Earth System Sciences Scale, USA Received: 1 August 2005 ­ Published in Hydrology and Earth System Sciences Discussions: 30 August

Boyer, Edmond

13

Aspects of Hess' Acquisition of American Oil & Gas  

Reports and Publications (EIA)

On July 27, 2010, Hess Corporation announced that it had agreed to acquire American Oil & Gas, Inc. in a stock-only transaction worth as much as $488 million (based on Hess' closing price of $53.30/share, anticipated number of newly issued shares, and $30 million credit facility extended to American Oil & Gas prior to closing).

2010-01-01T23:59:59.000Z

14

E-Print Network 3.0 - amerada hess corp Sample Search Results  

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

and Medicine 45 GEOPHYSICS, VOL. 60, NO. 2 (MARCH-APRIL 1995); P. 580488, 8 FIGS. Limited-view diffraction tomography in a Summary: (Grant no. 13 220), and partly by the...

15

Sequential decoupling of negative-energy states in Douglas-Kroll-Hess theory  

E-Print Network [OSTI]

Here, we review the historical development, current status, and prospects of Douglas--Kroll--Hess theory as a quantum chemical relativistic electrons-only theory.

Reiher, Markus

2015-01-01T23:59:59.000Z

16

Hess to serve on editorial advisory board | EMSL  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsruc DocumentationP-SeriesFlickr FlickrGuidedCH2M HILL SecretaryHazmatHelping Those inHenryHess to

17

Stochastic Acceleration in the Galactic Center HESS Source  

E-Print Network [OSTI]

Stochastic acceleration of electrons interacting resonantly with a turbulent magnetic field in a small accretion torus appears to be the likely mechanism responsible for much of Sagittarius A*'s millimeter and shorter wavelength spectrum. The longer wavelength radiation is produced at larger radii by electrons either diffusing from smaller scales or accelerated in situ. An important prediction of this model is the ejection of a significant flux of relativistic protons from a magnetic-field-dominated acceleration site into the wind-shocked medium surrounding the black hole. Recently, several air Cerenkov telescopes, notably HESS, have detected TeV emission from the Galactic center, with characteristics hinting at a p-p-induced pion decay process for the \\gamma-ray emission. Given (1) the size of this acceleration region measured in the radio band and (2) the wind-injected ISM mapped with Chandra using the diffuse X-rays, it is feasible to test the idea that protons accelerated within \\~20 Schwarzschild radii of the black hole produce the TeV emission farther out. We show a fraction of TeV protons scattering about once within ~3 pc of Sagittarius A* and the proton power (~10^37 erg s^-1) produced in concert with the 7 mm radio emission matches the TeV luminosity well. This model explains why the TeV source does not vary on a timescale of a year or less. The particle cascade generated by the p-p scatterings also produces bremsstrahlung, inverse Compton, and synchrotron emission at longer wavelengths from secondary particles. We compare these with current measurements and demonstrate that GLAST will detect this source during its one-year all-sky survey.

Siming Liu; Fulvio Melia; Vahe Petrosian; Marco Fatuzzo

2006-09-16T23:59:59.000Z

18

VERY LONG BASELINE INTERFEROMETRY SEARCH FOR THE RADIO COUNTERPART OF HESS J1943+213  

SciTech Connect (OSTI)

HESS J1943+213, a TeV point source close to the Galactic plane recently discovered by the H.E.S.S. Collaboration, was proposed to be an extreme BL Lacertae object, though a pulsar wind nebula (PWN) nature could not be completely discarded. To investigate its nature, we performed high-resolution radio observations with the European Very Long Baseline Interferometry Network (EVN) and reanalyzed archival continuum and H I data. The EVN observations revealed a compact radio counterpart of the TeV source. The low brightness temperature and the resolved nature of the radio source are indications against the beamed BL Lacertae hypothesis. The radio/X-ray source appears immersed in a {approx}1' elliptical feature, suggesting a possible galactic origin (PWN nature) for the HESS source. We found that HESS J1943+213 is located in the interior of a {approx}1 Degree-Sign diameter H I feature and explored the possibility of them being physically related.

Gabanyi, K. E. [Konkoly Observatory, Research Centre for Astronomy and Earth Sciences of the Hungarian Academy of Sciences, P.O. Box 67, Budapest H-1525 (Hungary)] [Konkoly Observatory, Research Centre for Astronomy and Earth Sciences of the Hungarian Academy of Sciences, P.O. Box 67, Budapest H-1525 (Hungary); Dubner, G.; Giacani, E. [Instituto de Astronomia y Fisica del Espacio (CONICET-UBA), CC 67, Suc. 28, 1428 Buenos Aires (Argentina)] [Instituto de Astronomia y Fisica del Espacio (CONICET-UBA), CC 67, Suc. 28, 1428 Buenos Aires (Argentina); Paragi, Z.; Pidopryhora, Y. [Joint Institute for VLBI in Europe, Postbus 2, 7990 AA Dwingeloo (Netherlands)] [Joint Institute for VLBI in Europe, Postbus 2, 7990 AA Dwingeloo (Netherlands); Frey, S., E-mail: gabanyi@konkoly.hu [FOeMI Satellite Geodetic Observatory, P.O. Box 585, H-1592 Budapest (Hungary)

2013-01-01T23:59:59.000Z

19

VERITAS Observations of the Unidentified Point Source HESS J1943+213  

E-Print Network [OSTI]

The H.E.S.S. Galactic plane scan has revealed a large population of Galactic very high energy (VHE; E > 100 GeV) emitters. The majority of the galactic sources are extended and can typically be associated with pulsar wind nebulae (35%) and supernova remnants (21%), while some of the sources remain unidentified (31%). A much smaller fraction of point-like sources (5 in total, corresponding to 4%) are identified as gamma-ray binaries. Active galactic nuclei located behind the Galactic plane are also a potential source class. An active galaxy could be identified in the VHE regime by a point like extension, a high variability amplitude (up to a factor of 100) and a typically soft spectrum (due to absorption by the extra-galactic background light). Here we report on VERITAS observations of HESS J1943+213, an unidentified point source discovered to emit above 470 GeV during the extended H.E.S.S. Galactic plane scan. This source is thought to be a distant BL Lac object behind the Galactic plane and, though it exhibi...

,

2015-01-01T23:59:59.000Z

20

A Possible Link Between the Galactic Center HESS Source and Sgr A*  

E-Print Network [OSTI]

Recently, HESS and other air Cerenkov telescopes have detected a source of TeV gamma-rays coincident with the Galactic center. It is not yet clear whether the gamma-rays are produced via leptonic or hadronic processes, so it is important to consider possible acceleration sites for the charged particles which produce the gamma-rays. One exciting possibility for the origin of these particles is the central black hole, Sgr A*, where the turbulent magnetic fields close to the event horizon can accelerate protons to TeV energies. Using a realistic model of the density distribution in a 6 pc x 6 pc x 6pc cube at the Galactic center, we here calculate the trajectories followed by these TeV protons as they gyrate through the turbulent medium surrounding Sgr A*. Diffusing out from the black hole, the protons produce TeV gamma-rays via pi^0 decay following a collision with a proton in the surrounding medium. After following over 222,000 such trajectories, we find that the circumnuclear ring around Sgr A* can reproduce the observed 0.1-100 TeV HESS spectrum and flux if the protons are injected into this medium with an effective power-law index of 0.75, significantly harder than the observed photon index of 2.25. The total energy in the steady-state 1-40 TeV proton population surrounding Sgr A* is inferred to be approx 5x10^{45} ergs. Only 31% of the emitted 1-100 TeV protons encounter the circumnuclear torus, leaving a large flux of protons that diffuse outward to contribute to the Galactic ridge emission observed by HESS on scales of >~ 1 degree.

D. R. Ballantyne; Fulvio Melia; Siming Liu; Roland M. Crocker

2007-02-13T23:59:59.000Z

Note: This page contains sample records for the topic "amerada hess hess" 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

VHE gamma-ray Emitting Pulsar Wind Nebulae Discovered by H.E.S.S.  

SciTech Connect (OSTI)

Recent advances in very-high-energy (VHE) gamma-ray astronomy have opened a new observational window on the physics of pulsars. The high sensitivity of current imaging atmospheric Cherenkov telescopes, and in particular of the H.E.S.S. array, has already led to the discovery of about a dozen VHE-emitting pulsar wind nebulae (PWNe) and PWN candidates. These include the plerions in the composite supernova remnants MSH 15-52, G21.5-0.9, Kes 75, and Vela, two sources in the Kookaburra, and the nebula of PSR B1823-13. This VHE emission is generally interpreted as inverse Compton emission from the relativistic electrons and positrons accelerated by the pulsar and its wind; as such, it can yield a more direct spatial and spectral view of the accelerated particles than can be inferred from observations of their synchrotron emission. The VHE-emitting PWNe detected by the H.E.S.S. telescopes are reviewed and the implications for pulsar physics discussed.

Gallant, Y.A.; /Montpellier U.; Carrigan, S.; /Heidelberg, Max Planck Inst.; Djannati-Atai, A.; /APC, Paris; Funk, S.; /KIPAC, Menlo Park; Hinton, J.A.; /Leeds U.; Hoppe, S.; /Heidelberg, Max Planck Inst.; de Jager, O.C.; /Potchefstroom U.; Khelifi, B.; /Ecole Polytechnique; Komin, Nu.; /Montpellier U.; Kosack, K.; /Heidelberg, Max Planck Inst.; Lemiere, A. /APC, Paris; Masterson, C.; /Dublin Inst.

2008-06-05T23:59:59.000Z

22

Multi-Zone Modeling of the Pulsar Win Nebula HESS J1825-137  

SciTech Connect (OSTI)

The pulsar wind nebula associated with PSR J1826-1334, HESS J1825-137, is a bright very high energy source with an angular extent of {approx} 1{sup o} and spatially-resolved spectroscopic TeV measurements. The gamma-ray spectral index is observed to soften with increasing distance from the pulsar, likely the result of cooling losses as electrons traverse the nebula. We describe analysis of X-ray data of the extended nebula, as well as 3-D time-dependent spectral energy distribution modeling, with emphasis on the spatial variations within HESS J1825-137. The multi-wavelength data places significant constraints on electron injection, transport, and cooling within the nebula. The large size and high nebular energy budget imply a relatively rapid initial pulsar spin period of 13 {+-} 7 ms and an age of 40 {+-} 9 kyr. The relative fluxes of each VHE zone can be explained by advective particle transport with a radially decreasing velocity profile with v(r) {proportional_to} r{sup -0.5}. The evolution of the cooling break requires an evolving magnetic field which also decreases radially from the pulsar, B(r, t) {proportional_to} r{sup -0.7} E(t){sup 1/2}. Detection of 10 TeV flux {approx} 80 pc from the pulsar requires rapid diffusion of high energy particles with {tau}{sub esc} {approx} 90 (R/10 pc){sup 2}(E{sub e}/100TeV){sup -1} year, contrary to the common assumption of toroidal magnetic fields with strong magnetic confinement. The model predicts a rather uniform Fermi LAT surface brightness out to {approx} 1{sup o} from the pulsar, in good agreement with the recently discovered LAT source centered 0.5{sup o} southwest of PSR J1826-1334 with extension 0.6 {+-} 0.1{sup o}.

Van Etten, Adam; Romani, Roger W.; /Stanford U., Phys. Dept.

2011-11-08T23:59:59.000Z

23

11Frontier Science, June 16Frontier Science, June 16thth 2004, Frascati2004, Frascati The H.E.S.S. experimentThe H.E.S.S. experiment  

E-Print Network [OSTI]

11Frontier Science, June 16Frontier Science, June 16thth 2004, Frascati2004, Frascati The H-Ray Astronomy PCC/APC M. Punch, PCC/APC Collège de France for the H·E·S·S· Collaboration #12; 22Frontier Science, June 16Frontier Science, June 16thth 2004, Frascati2004, Frascati The H.E.S.S. experimentThe H

24

X-Ray Observations of Unidentified H.E.S.S. Gamma-Ray Sources  

SciTech Connect (OSTI)

In a survey of the inner part of the Galaxy, performed with the H.E.S.S. Instrument (High energy stereoscopic system) in 2004 and 2005, a large number of new unidentified very high energy (VHE) {gamma}-ray sources above an energy of 100 GeV was discovered. Often the {gamma}-ray spectra in these sources reach energies of up to {approx} 10 TeV. These are the highest energy particles ever attributed to single astrophysical objects. While a few of these sources can be identified at other wavebands, most of these sources remain unidentified so far. A positive identification of these new g-ray sources with a counterpart object at other wavebands requires (a) a positional coincidence between the two sources,( b) a viable {gamma}-ray emission mechanism and (c) a consistent multiwavelength behavior of the two sources. X-ray observations with satellites such as XMM-Newton, Chandra or Suzaku provide one of the best channels to studying these enigmatic {gamma}-ray sources at other wavebands, since they combine high angular resolution and sensitivity with the ability to access non-thermal electrons through their synchrotron emission. We therefore have started a dedicated program to investigate VHE {gamma}-ray sources with high-sensitivity X-ray instruments.

Funk, S.; /SLAC

2007-10-10T23:59:59.000Z

25

XMM-Newton Observations Reveal the X-ray Counterpart of the Very-high-energy gamma-ray Source HESS J1640-465  

SciTech Connect (OSTI)

We present X-ray observations of the as of yet unidentified very high-energy (VHE) {gamma}-ray source HESS J1640-465 with the aim of establishing a counterpart of this source in the keV energy range, and identifying the mechanism responsible for the VHE emission. The 21.8 ksec XMM-Newton observation of HESS J1640-465 in September 2005 represents a significant improvement in sensitivity and angular resolution over previous ASCA studies in this region. These new data show a hard-spectrum X-ray emitting object at the centroid of the H.E.S.S. source, within the shell of the radio Supernova Remnant (SNR) G338.3-0.0. This object is consistent with the position and flux previously measured by both ASCA and Swift-XRT but is now shown to be significantly extended. We argue that this object is very likely the counterpart to HESS J1640-465 and that both objects may represent the Pulsar Wind Nebula of an as of yet undiscovered pulsar associated with G338.3-0.0.

Funk, S.; Hinton, J.A.; Puhlhofer, G.; Aharonian, F.A.; Hofmann, W.; Reimer, O.; Wagner, S.; /KIPAC, Menlo Park /Heidelberg, Max Planck Inst. /Leeds U. /Dublin Inst. /Stanford U., HEPL; Funk, S.; Hinton, J.A.; Puehlhofer, G.; Aharonian, F.A.; Hofmann, W.; Reimer, O.; Wagner, S.

2007-03-05T23:59:59.000Z

26

Proceedings of ICRC 2001: 2896 c Copernicus Gesellschaft 2001 The central data acquisition system for the H.E.S.S. telescope system  

E-Print Network [OSTI]

to the software design. 1 Introduction The High Energy Stereoscopic System, H.E.S.S. is a next generation imaging radiometers, cloud scanners, and op- tical telescopes for controlling the atmospheric properties. The Data. The signals of each pixel of a camera are read out via a high gain and a low gain path with 10 bits dynamic

27

Semi-Blind Cancellation of IQ-Imbalances Matthias Hesse, Student Member, IEEE, Marko Mailand, Student Member, IEEE, Hans-Joachim Jentschel,  

E-Print Network [OSTI]

Semi-Blind Cancellation of IQ-Imbalances Matthias Hesse, Student Member, IEEE, Marko Mailand iterative blind source separation (IBSS) as well as information about the modulation scheme used (hence the term semi-blind). The novelty of our approach lies in the fact that we match the nonlinearity involved

Paris-Sud XI, Université de

28

Global MHD modeling of the impact of a solar wind pressure change Kristi A. Keller, Michael Hesse, Maria Kuznetsova, Lutz Rastatter, and Therese Moretto  

E-Print Network [OSTI]

Global MHD modeling of the impact of a solar wind pressure change Kristi A. Keller, Michael Hesse of Michigan, Ann Arbor, Michigan, USA Received 26 February 2001; revised 21 December 2001; accepted 21 December 2001; published 23 July 2002. [1] A sudden increase in the solar wind dynamic pressure compresses

De Zeeuw, Darren L.

29

The properties of the putative pulsar associated with IGR J18135-1751/HESS J1813-178  

E-Print Network [OSTI]

Context: We investigate the possible theoretical properties of the putative pulsar associated with the pulsar wind nebula IGR J18135-1751/HESS J1813-178 based upon recent gamma-ray observations and archival multi-wavelength observations. Aims: We show that when using the standard equations for magnetic dipole radiation with recent soft gamma-ray observations leads to deriving an extreme set of parameters (magnetic field, period and spin down rate) for the putative pulsar. Alternative scenarios that generate more typical parameter values are explored. Methods: The properties of the putative pulsar are calculated assuming that the 20-100 keV luminosity corresponds to 1% of Edot, that the source is 4.5 kpc away, and that the pulsar age is 300 yrs. This gives P = 0.55 s, Pdot = 3E-11 s/s, and B = 1.28E14 G. This is a very extreme set compared to the population of known pulsars in PWN systems. Using the equations for magnetic dipole losses makes it possible to adjust the initial assumptions to see what is required for a more reasonable set of pulsar parameters. Results: The current measured properties for IGR J18135-1751/HESS J1813-178 (i.e. luminosity, distance, and age) result in extreme properties of the unseen pulsar within the PWN. The simplest method for achieving more reasonable properties for the pulsar is to decouple the spin-down age of the pulsar from the actual age for the system.

A. J. Dean; A. B. Hill

2008-04-21T23:59:59.000Z

30

The 2012 flare of PG 1553+113 seen with H.E.S.S. and Fermi-LAT  

E-Print Network [OSTI]

Very high energy (VHE, $E>$100 GeV) $\\gamma$-ray flaring activity of the high-frequency peaked BL Lac object \\pg\\ has been detected by the \\hess\\ telescopes. The flux of the source increased by a factor of 3 during the nights of 2012 April 26 and 27 with respect to the archival measurements with hint of intra-night variability. No counterpart of this event has been detected in the \\fla\\ data. This pattern is consistent with VHE $\\gamma$ ray flaring being caused by the injection of ultrarelativistic particles, emitting $\\gamma$ rays at the highest energies. The dataset offers a unique opportunity to constrain the redshift of this source at \\bestz\\ using a novel method based on Bayesian statistics. The indication of intra-night variability is used to introduce a novel method to probe for a possible Lorentz Invariance Violation (LIV), and to set limits on the energy scale at which Quantum Gravity (QG) effects causing LIV may arise. For the subluminal case, the derived limits are $\\textrm{E}_{\\rm QG,1}>4.10\\times...

Abramowski, A; Benkhali, F Ait; Akhperjanian, A G; Angüner, E O; Backes, M; Balenderan, S; Balzer, A; Barnacka, A; Becherini, Y; Tjus, J Becker; Berge, D; Bernhard, S; Bernlöhr, K; Birsin, E; Biteau, J; Böttcher, M; Boisson, C; Bolmont, J; Bordas, P; Bregeon, J; Brun, F; Brun, P; Bryan, M; Bulik, T; Carrigan, S; Casanova, S; Chadwick, P M; Chakraborty, N; Chalme-Calvet, R; Chaves, R C G; Chrétien, M; Colafrancesco, S; Cologna, G; Conrad, J; Couturier, C; Cui, Y; Dalton, M; Davids, I D; Degrange, B; Deil, C; deWilt, P; Djannati-Ataï, A; Domainko, W; Donath, A; Drury, L O'C; Dubus, G; Dutson, K; Dyks, J; Dyrda, M; Edwards, T; Egberts, K; Eger, P; Espigat, P; Farnier, C; Fegan, S; Feinstein, F; Fernandes, M V; Fernandez, D; Fiasson, A; Fontaine, G; Förster, A; Fü\\ssling, M; Gabici, S; Gajdus, M; Gallant, Y A; Garrigoux, T; Giavitto, G; Giebels, B; Glicenstein, J F; Gottschall, D; Grondin, M -H; Grudzi?ska, M; Hadsch, D; Häffner, S; Hahn, J; Harris, J; Heinzelmann, G; Henri, G; Hermann, G; Hervet, O; Hillert, A; Hinton, J A; Hofmann, W; Hofverberg, P; Holler, M; Horns, D; Ivascenko, A; Jacholkowska, A; Jahn, C; Jamrozy, M; Janiak, M; Jankowsky, F; Jung, I; Kastendieck, M A; Katarzy?ski, K; Katz, U; Kaufmann, S; Khélifi, B; Kieffer, M; Klepser, S; Klochkov, D; Klu?niak, W; Kolitzus, D; Komin, Nu; Kosack, K; Krakau, S; Krayzel, F; Krüger, P P; Laffon, H; Lamanna, G; Lefaucheur, J; Lefranc, V; Lemière, A; Lemoine-Goumard, M; Lenain, J -P; Lohse, T; Lopatin, A; Lu, C -C; Marandon, V; Marcowith, A; Marx, R; Maurin, G; Maxted, N; Mayer, M; McComb, T J L; Méhault, J; Meintjes, P J; Menzler, U; Meyer, M; Mitchell, A M W; Moderski, R; Mohamed, M; Morå, K; Moulin, E; Murach, T; de Naurois, M; Niemiec, J; Nolan, S J; Oakes, L; Odaka, H; Ohm, S; Opitz, B; Ostrowski, M; Oya, I; Panter, M; Parsons, R D; Arribas, M Paz; Pekeur, N W; Pelletier, G; Perez, J; Petrucci, P -O; Peyaud, B; Pita, S; Poon, H; Pühlhofer, G; Punch, M; Quirrenbach, A; Raab, S; Reichardt, I; Reimer, A; Reimer, O; Renaud, M; Reyes, R de los; Rieger, F; Rob, L; Romoli, C; Rosier-Lees, S; Rowell, G; Rudak, B; Rulten, C B; Sahakian, V; Salek, D; Sanchez, D A; Santangelo, A; Schlickeiser, R; Schüssler, F; Schulz, A; Schwanke, U; Schwarzburg, S; Schwemmer, S; Sol, H; Spanier, F; Spengler, G; Spies, F; Stawarz, ?; Steenkamp, R; Stegmann, C; Stinzing, F; Stycz, K; Sushch, I; Tavernet, J -P; Tavernier, T; Taylor, A M; Terrier, R; Tluczykont, M; Trichard, C; Valerius, K; van Eldik, C; van Soelen, B; Vasileiadis, G; Veh, J; Venter, C; Viana, A; Vincent, P; Vink, J; Völk, H J; Volpe, F; Vorster, M; Vuillaume, T; Wagner, P; Wagner, R M; Ward, M; Weidinger, M; Weitzel, Q; White, R; Wierzcholska, A; Willmann, P; Wörnlein, A; Wouters, D; Yang, R; Zabalza, V; Zaborov, D; Zacharias, M; Zdziarski, A A; Zech, A; Zechlin, H -S

2015-01-01T23:59:59.000Z

31

Detection of VHE gamma-ray emission from the distant blazar 1ES 1101-232 with H.E.S.S. and broadband characterisation  

E-Print Network [OSTI]

The blazar 1ES 1101-232 was observed with the High Energy Stereoscopic System (H.E.S.S.) of Atmospheric Cherenkov Telescopes (ACT) in 2004 and 2005, for a live time of 43 hours. VHE (E > 10^11 eV) gamma-rays were detected for the first time from this object. VHE observations of blazars are used to investigate the inner parts of the blazar jets, and also to study the extragalactic background light (EBL) in the near-infrared band. Observations in 2005 were conducted in a multiwavelength campaign, together with the RXTE satellite and optical observations. In 2004, simultaneous observations with XMM-Newton were obtained. 1ES 1101-232 was detected with H.E.S.S. with an excess of 722 photons, at a significance of 12 sigma. The measured VHE gamma-ray flux amounts to dN/dE = (5.63 +- 0.89) x 10^-13 (E/TeV)^-(2.94 +- 0.20) cm^-2 s^-1 TeV^-1, above a spectral energy threshold of 225 GeV. No significant variation of the VHE gamma-ray flux on any time scale was found. 1ES 1101-232 exhibits a very hard spectrum, and at a ...

Akhperjanian, A G; Beilicke, M; Benbow, W; Berge, D; Bernlöhr, K; Boisson, C; Bolz, O; Borrel, V; Braun, I; Brion, E; Brown, A M; Buhler, R; Büsching, I; Boutelier, T; Carrigan, S; Chadwick, P M; Chounet, L M; Coignet, G; Cornils, R; Costamante, L; Degrange, B; Dickinson, H J; Djannati-Atai, A; O'Connor-Drury, L; Dubus, G; Egberts, K; Emmanoulopoulos, D; Espigat, P; Farnier, C; Feinstein, F; Ferrero, E; Fiasson, A; Fontaine, G; Funk, Seb; Funk, S; Fussling, M; Gallant, Y A; Giebels, B; Glicenstein, J F; Glück, B; Goret, P; Hadjichristidis, C; Hauser, D; Hauser, M; Heinzelmann, G; Henri, G; Hermann, G; Hinton, J A; Hoffmann, A; Hofmann, W; Holleran, M; Hoppe, S; Horns, D; Jacholkowska, A; De Jager, O C; Kendziorra, E; Kerschhaggl, M; Khelifi, B; Komin, Nu; Kosack, K; Lamanna, G; Latham, I J; Le Gallou, R; Lemiere, A; Lemoine-Goumard, M; Lohse, T; Martin, J M; Martineau-Huynh, O; Marcowith, A; Masterson, C; Maurin, G; McComb, T J L; Moulin, E; De Naurois, Mathieu; Nedbal, D; Nolan, S J; Noutsos, A; Olive, J P; Orford, K J; Osborne, J L; Panter, M; Pelletier, G; Petrucci, P O; Pita, S; Pühlhofer, G; Punch, M; Ranchon, S; Raubenheimer, B C; Raue, M; Rayner, S M; Ripken, J; Rob, L; Rolland, L; Rosier-Lees, S; Rowell, G; Sahakian, V V; Santangelo, A; Sauge, L; Schlenker, S; Schlickeiser, R; Schroder, R; Schwanke, U; Schwarzburg, S; Schwemmer, S; Shalchi, A; Sol, H; Spangler, D; Spanier, F; Steenkamp, R; Stegmann, C; Superina, G; Tam, P H; Tavernet, J P; Terrier, R; Tluczykont, M; Van Eldik, C; Vasileiadis, G; Venter, C; Vialle, J P; Vincent, P; Völk, H J; Wagner, S J; Ward, M

2007-01-01T23:59:59.000Z

32

Nancy J. Hess | EMSL  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the Contributions andData andFleet TestAccounts andThe Role of MesoscaleNancy IsernNancy

33

Michael Hess | Department of Energy  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "of EnergyEnergyENERGYWomen OwnedofDepartment ofJared Temanson -ofMarc MorialMegan Slack

34

Upgrading Amerada-type survey clocks for high-temperature geothermal service  

SciTech Connect (OSTI)

The Amerada type subsurface recording gauges have been used by the oil and gas industry for many years. These mechanical logging instruments are currently used by the growing goethermal industry. As the gauges were designed for service in low-temperature oil and gas wells, a significant number of failures are occurring at elevated geothermal temperatures. The spring driven mechanical survey clocks appear to be the primary cause of the failures. The clock mechanisms tend to stop or lock-up when exposed to temperatures as high as 300/sup 0/C. This paper summarizes a project that was undertaken to upgrade the survey clocks to 300/sup 0/C capability. The major problems causing clock failure were indentified and corrected by straightforward design modifications together with special lubrication of the moving parts. Several clocks so modified performed reliably, both during laboratory oven tests and during field tests that were performed in actual geothermal wells at temperatures up to 330/sup 0/C.

Major, B.H.; Witten, C.L.

1980-09-01T23:59:59.000Z

35

Thomas E. Hess Page 1 5/19/14 Thomas Hess  

E-Print Network [OSTI]

software QA, testing, knowledge management, training, worldwide customer support and critical problem, when optimally complied, dramatically increased the speed of end user experience and program execution implementation changes. As a result of this development, the "GeoFrame" product was significantly increased

Yang, Zong-Liang

36

PHILIPPE-JEAN HESSE JEAN-PIERRE LE CROM  

E-Print Network [OSTI]

, Paris, IHTP et CRHMSS, 1992, pp. 335-342 ; Jean Bennet, « La mutualité pendant la Seconde Guerre

Paris-Sud XI, Université de

37

Hybrid energy systems (HESs) using small modular reactors (SMRs)  

SciTech Connect (OSTI)

Large-scale nuclear reactors are traditionally operated for a singular purpose: steady-state production of dispatchable baseload electricity that is distributed broadly on the electric grid. While this implementation is key to a sustainable, reliable energy grid, small modular reactors (SMRs) offer new opportunities for increased use of clean nuclear energy for both electric and thermal ap plications in more locations – while still accommodating the desire to support renewable production sources.

S. Bragg-Sitton

2014-10-01T23:59:59.000Z

38

SUR LES DILECTRIQUES HTROGNES; PAR M. A. HESS.  

E-Print Network [OSTI]

~'~,~ ... lenrs pouvoirs inducteurs et r, t,', r~ ... leurs résis- tances spécifiqu es : Dans le cas particulier

Paris-Sud XI, Université de

39

Hess Retail Natural Gas and Elec. Acctg. (Connecticut) | Open Energy  

Open Energy Info (EERE)

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Office of InspectorConcentrating Solar Power BasicsGermany: EnergyPower Finance

40

Hess Retail Natural Gas and Elec. Acctg. (Delaware) | Open Energy  

Open Energy Info (EERE)

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Office of InspectorConcentrating Solar Power BasicsGermany: EnergyPower FinanceInformation Delaware References: EIA

Note: This page contains sample records for the topic "amerada hess hess" 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

Hess Retail Natural Gas and Elec. Acctg. (Maryland) | Open Energy  

Open Energy Info (EERE)

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Office of InspectorConcentrating Solar Power BasicsGermany: EnergyPower FinanceInformation DelawareInformation

42

Hess Retail Natural Gas and Elec. Acctg. (Massachusetts) | Open Energy  

Open Energy Info (EERE)

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Office of InspectorConcentrating Solar Power BasicsGermany: EnergyPower FinanceInformation

43

Hess Retail Natural Gas and Elec. Acctg. (Pennsylvania) | Open Energy  

Open Energy Info (EERE)

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Office of InspectorConcentrating Solar Power BasicsGermany: EnergyPower

44

Hydrology and Earth System Sciences, 9, 95109, 2005 www.copernicus.org/EGU/hess/hess/9/95/  

E-Print Network [OSTI]

varying little from year to year. For hydroelectricity production, the water management therefore rather

Paris-Sud XI, Université de

45

Hydrology and Earth System Sciences, 9, 535547, 2005 www.copernicus.org/EGU/hess/hess/9/535/  

E-Print Network [OSTI]

areas, irrigation serves to increase yields, to at- tenuate the effects of droughts or, in the case), Germany 2Food and Agriculture Organization of the United Nations, Rome, Italy Received: 16 June 2005 land cover inventories. 1 Introduction Agriculture is by far the largest water-use sector, accounting

Paris-Sud XI, Université de

46

A dense gas survey of the gamma-ray sources HESS J1731-347 and HESS J1729-345  

E-Print Network [OSTI]

The results of Mopra molecular spectral line observations towards the supernova remnant HESSJ1731-347 (G353.6-0.7) and the unidentified gamma-ray source HESSJ1729-345 are presented. Dense molecular gas in three different velocity-bands (corresponding to three Galactic arms) are investigated using the CS(1-0) line. The CS-traced component provides information about the dense target material in a hadronic scenario for gamma-ray production (cosmic rays interacting with gas) and an understanding of the dynamics. Furthermore, the effects of cosmic ray diffusion into dense gas may alter the gamma-ray spectrum to cause a flattening of spectra towards such regions. Dense molecular gas mass at a level of ~10^5 Mo was revealed in this survey, with mass of the order of ~10^3 Mo towards HESSJ1729-345 in each coincident Galactic arm, but no significant detection of dense molecular gas towards HESSJ1731-347 at the currently-preferred distance of ~5.2-6.2 kpc was discovered.

Maxted, Nigel; de Wilt, Phoebe; Burton, Michael; Renaud, Matthieu; Fukui, Yasuo; Hawkes, Jarryd; Blackwell, Rebecca; Voisin, Fabien; Lowe, Vicki; Aharonian, Felix

2015-01-01T23:59:59.000Z

47

Mario Hess, Bernadine Strik, Jason Smesrud, and John Selker November 1997 Department of Bioresource Engineering  

E-Print Network [OSTI]

they are shallow-rooted, strawberries are subject to drought injury. A uniform and adequate supply of mo isture development (strawberry fruit is about 90% water). Water stress at this time results in small fruit size of fruit rot. On medium- and heavy-textured soils, a good rain or irrigation just before the first picking

Selker, John

48

Jason Smesrud, Bill Mansour, Mario Hess, and John Selker November 1997 Department of Bioresource Engineering  

E-Print Network [OSTI]

excessive stalk and leaf mass. The use of big guns and center pivot systems is common in corn due to difficulties in moving pipe as fields approach maturity. When using big guns, it is critical to pay close

Selker, John

49

10 Questions for a Spectroscopy Expert: Nancy Hess | Department of Energy  

Energy Savers [EERE]

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious RankCombustion |Energyon ArmedWaste and Materials Disposition#EnergyFaceoff1 1 1 More

50

Hess Retail Natural Gas and Elec. Acctg. (District of Columbia) | Open  

Open Energy Info (EERE)

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Office of InspectorConcentrating Solar Power BasicsGermany: EnergyPower FinanceInformation Delaware References:

51

Hess Retail Natural Gas and Elec. Acctg. (Maine) | Open Energy Information  

Open Energy Info (EERE)

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Office of InspectorConcentrating Solar Power BasicsGermany: EnergyPower FinanceInformation Delaware

52

Hess Retail Natural Gas and Elec. Acctg. (New Hampshire) | Open Energy  

Open Energy Info (EERE)

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Office of InspectorConcentrating Solar Power BasicsGermany: EnergyPower FinanceInformationInformation Hampshire

53

Hess Retail Natural Gas and Elec. Acctg. (New York) | Open Energy  

Open Energy Info (EERE)

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Office of InspectorConcentrating Solar Power BasicsGermany: EnergyPower FinanceInformationInformation

54

Hess Retail Natural Gas and Elec. Acctg. (Rhode Island) | Open Energy  

Open Energy Info (EERE)

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Office of InspectorConcentrating Solar Power BasicsGermany: EnergyPowerInformation Rhode Island References: EIA

55

Organophosphates as Solvents for Electrolytes in Electrochemical Andrew Hess, Greg Barber, Chen Chen, Thomas E. Mallouk, and Harry R. Allcock*  

E-Print Network [OSTI]

that employ liquid electrolytes for solar power conversion and energy storage, respectively.1,2 Although these problems. DSSCs are also a promising alternative to silicon-based solar cells due to their low raw-sensitized solar cells (DSSCs) and secondary lithium batteries. Unoptimized DSSC electrolyte formulations for DSSCs

56

eHealth Research from the User's Perspective Bradford W. Hesse, PhD, Ben Shneiderman, PhD  

E-Print Network [OSTI]

people do?" How can eHealth take part in national goals for healthcare reform to empower relationships (IT) to issues of personal health and health care has had a long and surprisingly complex history of IT applied to health care reflect the lessons learned from computer science more generally. The field

Shneiderman, Ben

57

A Novel Routing Metric for Environmentally-Powered Sensors With Hybrid  

E-Print Network [OSTI]

an Hybrid Energy Storage System (HESS). An HESS is composed of a supercapacitor (SC) and a rechargeable storage system (HESS), in which a supercapacitor (SC) protects the battery from current spikes, is another

Ingram, Mary Ann

58

Salt dome discoveries mounting in Mississippi  

SciTech Connect (OSTI)

Exploratory drilling around piercement salt domes in Mississippi has met with a string of successes in recent months. Exploration of these salt features is reported to have been initiated through the review of non-proprietary, 2D seismic data and subsurface control. This preliminary data and work were then selectively upgraded by the acquisition of additional, generally higher quality, conventional 2D seismic lines. This current flurry of successful exploration and ensuing development drilling by Amerada Hess Corp. on the flanks of salt domes in Mississippi has resulted in a number of significant Hosston discoveries/producers at: Carson salt dome in Jefferson Davis County; Dry Creek salt dome in Covington County, Midway salt dome in lamar County, Monticello salt dome in Lawrence County, and Prentiss salt dome in Jefferson Davis County. The resulting production from these fields is gas and condensate, with wells being completed on 640 acre production units.

Ericksen, R.L. [Mississippi Office of Geology, Jackson, MS (United States)

1996-06-17T23:59:59.000Z

59

The shape and size of crowding for moving targets Peter J. Bex *, Steven C. Dakin, Anita J. Simmers  

E-Print Network [OSTI]

(Bondarko & Danilova, 1997; Hess, Dakin, & Kapoor, 2000). How- ever, crowding also occurs between target

Bex, Peter

60

E-Print Network 3.0 - andis auhinna soome Sample Search Results  

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

1 A sgn(v) o... ) Coulumb+viscous e) Karnopp c) Coulumb+viscous+stiction f) Hess and Soom Armstrong, etc 12... Friction Friction velocity lag time Hess and Soom (1990): F(v; t) ...

Note: This page contains sample records for the topic "amerada hess hess" 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

Helping people 2 Johnson Controls September 18, 2013  

E-Print Network [OSTI]

Johnson Controls 4 Ford Motor Co. 5 Intel Corp. 6 Hess Corp. 7 Air Products & Chemicals 8 Praxair Inc. 9

Subramanian, Venkat

62

Atmos. Chem. Phys., 14, 609627, 2014 www.atmos-chem-phys.net/14/609/2014/  

E-Print Network [OSTI]

convection (Lawrence et al., 2003; Liu et al., 2003; Hess, 2005; Halland et al., 2009; Zhao et al., 2009

Meskhidze, Nicholas

63

Early and later diagenetic alteration of Ordovician Red River carbonates, Tioga Deep field, Williston basin, North Dakota  

SciTech Connect (OSTI)

The Ordovician Red River Formation in the Williston basin is generally subdivided into three restrictive-upward cycles referred to as 'A,' 'B,' and 'C' zones in descending order. Most Red River production in western North Dakota and eastern Montana comes from dolomitized burrowed and laminated members of the C-cycle. Four cores taken by Amerada Hess Corporation within the Tioga Deep field, Williams and Montrail Counties, North Dakota, were studied in detail to establish depositional and diagenetic controls on porosity distribution within the Red River. Dolomitized portions of the Red River C member are genetically related to downward-descending Mg-rich brines derived from hypersaline basin waters depleted of their sulfate content throught attendant precipitation of gypsum. Calcite associated with this early dolomitization phase occupied intercrystalline positions between dolomite rhombs. Following burial, limestones tended to chemically compact through pressure solution, whereas late stage fractures were localized in the more brittle dolomitic portions of the Red River. These fractures served as conduits for late stage leaching fluids, possibly associated with hydrocarbon generation, that enhanced porosity in the dolomites through the removal of associated calcite. Late-stage leaching is reflected in 'overly porous' dolomite haloes around cemented burrow centers and highly porous dolomite seams along stylolitic contacts. Previous models proposed to explain porosity distribution within Red River reservoirs should be modified to include the overprint of deep diagenetic effects.

Perkins, R.D. (Duke Univ., Durham, NC (United States))

1991-03-01T23:59:59.000Z

64

98:537-541, 2007. First published Apr 18, 2007; doi:10.1152/jn.01229.2006J Neurophysiol Eliana M. Klier, Dora E. Angelaki and Bernhard J. M. Hess  

E-Print Network [OSTI]

of the nervous system. It is published 12 times a yearJournal of Neurophysiology onFebruary19,2009jn rotations about different axes--yaw, pitch, and roll. The order in which we rotate about these axes are accurate after intervening, whole-body rotational sequences. The sequences were reversed, either yaw

Crawford, Doug

65

Murray Gell-Mann den ttafaldiga  

E-Print Network [OSTI]

Murray Gell-Mann och den åttafaldiga vägen Kathryn Hess Lite partikelteori Matriser och Lie-algebror Representationer av Lie-algebror Murray Gell-Mann och den åttafaldiga vägen Kathryn Hess Institute of Geometry november 2008 #12;Murray Gell-Mann och den åttafaldiga vägen Kathryn Hess Lite partikelteori Matriser och

Thévenaz, Jacques

66

Constraints on the TeV source population and its contribution to the galactic diffuse TeV emission  

E-Print Network [OSTI]

The detection by the HESS atmospheric Cerenkov telescope of fourteen new sources from the Galactic plane makes it possible to estimate the contribution of unresolved sources like those detected by HESS to the diffuse Galactic emission measured by the Milagro Collaboration. The number-intensity relation and the luminosity function for the HESS source population are investigated. By evaluating the contribution of such a source population to the diffuse emission we conclude that a significant fraction of the TeV energy emission measured by the Milagro experiment could be due to unresolved sources like HESS sources. Predictions concerning the number of sources which Veritas, Milagro, and HAWC should detect are also given.

Casanova, Sabrina

2007-01-01T23:59:59.000Z

67

Enhanced High Temperature Performance of NOx Storage/Reduction...  

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

Neal Currier, Junhui Li, Alex Yezerets Cummins Inc. Hai-Ying Chen, Howard Hess Johnson Matthey ACE026 2 Project Overview Timeline Budget Partners Barriers * Start - March...

68

Mechanisms of Sulfur Poisoning of NOx Adsorber (LNT) Materials  

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

Stafford, John Stang (retired), Alex Yezerets Cummins Inc. Hai-Ying Chen, Howard Hess Johnson Matthey Project ID: ace24peden 2 Project Overview Timeline Budget Partners Barriers...

69

Enhanced High and Low Temperature Performance of NOx Reduction...  

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

Junhui Li, Alex Yezerets Cummins Inc. Mario Castagnola, Hai-Ying Chen, Howard Hess Johnson Matthey ACE026 2 Project Overview Timeline Budget Partners Barriers * Start - March...

70

Enhanced High Temperature Performance of NOx Storage/Reduction...  

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

Neal Currier, Junhui Li, Alex Yezerets Cummins Inc. Hai-Ying Chen, Howard Hess Johnson Matthey Ace026 2 Project Overview Timeline Budget Partners Barriers * Start - July...

71

Approaches To Integrating A HIgh Penertration Of Solar PV and CPV Onto The Electrical Grid  

E-Print Network [OSTI]

Happy Camp Sanitation District  Harwood Products, Inc.   Healdsburg City  Herlong PUD  Hess Collection Winery  Hidden Valley 

Hill, Steven Craig

2013-01-01T23:59:59.000Z

72

Constraints on the TeV source population and its contribution to the galactic diffuse TeV emission  

E-Print Network [OSTI]

The detection by the HESS atmospheric Cerenkov telescope of fourteen new sources from the Galactic plane makes it possible to estimate the contribution of unresolved sources like those detected by HESS to the diffuse Galactic emission measured by the Milagro Collaboration. The number-intensity relation and the luminosity function for the HESS source population are investigated. By evaluating the contribution of such a source population to the diffuse emission we conclude that a significant fraction of the TeV energy emission measured by the Milagro experiment could be due to unresolved sources like HESS sources. Predictions concerning the number of sources which Veritas, Milagro, and HAWC should detect are also given.

Sabrina Casanova; Brenda L. Dingus

2007-11-19T23:59:59.000Z

73

Photon stimulated desorption from KI: Laser control of I-atom...  

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

M Henyk AG Joly KM Beck WP Hess Capabilities: Spectroscopy and Diffraction NMR and EPR Facility: Radiochemistry Annex Science Theme: Energy Materials & Processes Terrestrial...

74

E-Print Network 3.0 - automatic local gabor Sample Search Results  

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

orientation Harriet A. Allen, Robert F. Hess, and Behzad Mansouri Summary: of Gabors, a task requiring that the visual system combine local estimates of orientation across space......

75

President Obama Announces New Public-Private Manufacturing Innovation...  

Office of Environmental Management (EM)

Gridbridge, Hesse Mechantronics, II-VI, IQE, John Deere, Monolith Semiconductor, RF Micro Devices, Toshiba International, Transphorm, USCi, Vacon 7 Universities and Labs:...

76

Power Maps in Algebra and  

E-Print Network [OSTI]

Power Maps in Algebra and Topology Kathryn Hess Preface The case of commutative algebras The Hochschild complex of a twisting cochain Power maps on the Hochschild complex Topological relevance Power Compostela, 17 September 2008 #12;Power Maps in Algebra and Topology Kathryn Hess Preface The case

Thévenaz, Jacques

77

Discovery of two candidate pulsar wind nebulae in very-high-energy gamma rays  

E-Print Network [OSTI]

We present the discovery of two very-high-energy gamma-ray sources in an ongoing systematic search for emission above 100 GeV from pulsar wind nebulae in survey data from the H.E.S.S. telescope array. Imaging Atmospheric Cherenkov Telescopes are ideal tools for searching for extended emission from pulsar wind nebulae in the very-high-energy regime. H.E.S.S., with its large field of view of 5 degrees and high sensitivity, gives new prospects for the search for these objects. An ongoing systematic search for very-high-energy emission from energetic pulsars over the region of the Galactic plane between -60 degrees wind nebulae, HESS J1718-385 and HESS J1809-193. H.E.S.S. has proven to be a suitable instrument for pulsar wind nebula searches.

H. E. S. S. Collaboration; :; F. Aharonian

2007-05-11T23:59:59.000Z

78

Independent Scientific Advisory Board Review of Salmon and Steelhead  

E-Print Network [OSTI]

Hoc Member Richard N. Williams -ISRP #12;Acknowledgements The ISAB thanks all of the scientists Hallerman, Pete Hassemer, Jay Hesse, Ray Hilborn, Mike Kern, Paul Kline, Jim Lannan, Si Levin, Jeff Lutch

79

CCSM Atmosphere Model Working Group Report, 22-24 March 2006  

E-Print Network [OSTI]

, Aiguo Donner, Leo Eaton, Brian Gent, Peter Gettelman, Andrew Ghan, Steven J Hack, James Hannay, Cecile, Colette L. Hess, Peter Heymsfeld, Andrew Liu, Hongyu Neu, Jessica Rodriguez, Jose M. Vit

80

HEADING FRONTMATTER  

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

3, Edited by Mustafa Ali Mohd, Intech Publishers, ISBN 979-953-307-737-5. 8. Hess, J.R.; Kenney, K.L.; Wright, C.T.; Perlack, R.; and Turhollow, A. (2009). Corn Stover...

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81

CFSES Blue Team Presentations  

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

Field Marc Hesse (May, 2014) Nanoscale CO2-brine-mineral interactions Craig M. Tenney, Randall T. Cygan, Evgeniy M. Myshakin, Wissam A. Saidi, Vyacheslav N. Romanov, and Kenneth D....

82

Interfacial ionic liquids: connecting static and dynamic...  

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

L, Lee S S and Fenter P 2012 Real-time observations of interfacial lithiation in a metal silicide thin film J. Phys. Chem. C 116 22341-5 43 Lindahl E, Hess B and van der...

83

Universittsmedizin Gttingen Publikationen und Hochschulschriften 2010  

E-Print Network [OSTI]

-assisted image-guided transcranial magnetic stimulation for somatotopic mapping of the motor cortex: a clinical Volumensequenzen bei 3 Tesla. Dissertation Universität Göttingen 2010. 2. Hesse A, Dr. med., Untersuchung neuer

Gollisch, Tim

84

Contribution of unresolved point sources to the galactic diffuse emission  

E-Print Network [OSTI]

The detection by the HESS atmospheric Cherenkov telescope of fifteen new sources from the Galactic plane makes it possible to estimate the contribution of unresolved point sources like those detected by HESS to the diffuse Galactic emission measured by EGRET and recently at higher energies by the Milagro Collaboration. Assuming that HESS sources have all the same intrinsic luminosity, the contribution of this new source population can account for most of the Milagro $\\gamma$-ray emission at TeV energies and between 10 and 20 per cent of EGRET diffuse Galactic $\\gamma$-ray emission for energies bigger than 10 GeV. Also, by combining the HESS and the Milagro results, constraints can be put on the distribution and the luminosities of gamma ray emitters in the Galaxy.

Casanova, S; Casanova, Sabrina; Dingus, Brenda L.

2006-01-01T23:59:59.000Z

85

Microsoft Word - TM2012-003-0 35 dollar in TM format .docx  

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

Cellulose, 16:599-619. Hess, J.R., Wright C.T., Kenney K.L. 2007. Cellulosic Biomass Feedstocks and Logistics for Ethanol Production. Biofuels, Bioproducts and Biorefining,...

86

Ultracapacitor/Battery Hybrid Energy Storage Systems for Electric Vehicles.  

E-Print Network [OSTI]

??This thesis deals with the design of Hybrid Energy Storage System (HESS) for Light Electric Vehicles (LEV) and EVs. More specifically, a tri-mode high-efficiency non-isolated… (more)

Moshirvaziri, Mazhar

2012-01-01T23:59:59.000Z

87

E-Print Network 3.0 - automatic mirror alignment Sample Search...  

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

for: automatic mirror alignment Page: << < 1 2 3 4 5 > >> 1 The Universe Viewed in Gamma-Rays 1 Mirror Alignment and Optical Quality of the H.E.S.S. Summary: the automatic...

88

Passive Catalytic Approach to Low Temperature NOx Emission Abatement  

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

Aleksey Yezerets, Michael Ruth Cummins Inc. Hai-Ying Chen, Howard Hess, Mojghan Naseri Johnson Matthey 10252011 US DoE DEER Conference 2011 * 40% Fuel Economy improvement over...

89

Mechanisms of Sulfur Poisoning of NOx Adsorber (LNT) Materials  

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

Stafford, Junhui Li, John Stang, Alex Yezerets Cummins Inc. Hai-Ying Chen, Howard Hess Johnson Matthey 2 The project is a CRADA between PNNL and Cummins Inc. It involves a...

90

GEOPHYSICAL RESEARCH LETTERS, VOL. 28, NO. 24, PAGES 4631-4634, DECEMBER 15, 2001 Remote sensing of global wetland dynamics with  

E-Print Network [OSTI]

and a linear mixture model with end-members calibrated with radar observations to account for vegetation cover-arid environments [Gumbricht et al., personal communication]. Synthetic aper- ture radar (SAR) studies [Hess et al

Aires, Filipe

91

Clin. Vision Sci. Vol. 2, No. 3, pp. 143-158, 1988 Printed in Great Britain. All rights reserved  

E-Print Network [OSTI]

CLOUDY MEDIA D. KERSTEN Psychology Department, Brown University, Providence, RI 02912, U.S.A. R. F. HEss imposed by the receptor spacing (Campbell and Green, 1965). As Green points out, in practice it can

Kersten, Dan

92

Table of Contents Invited Talks  

E-Print Network [OSTI]

Shih, Keith Sklower, Lakshminarayanan Subramanian, Takashi Suzuki, Shelley Zhuang, Anthony D. Joseph . . . . . . . . . . 16 Christopher K. Hess, Manuel Rom´an, Roy H. Campbell Systems Support for Ubiquitous Computing . . . . . . . . . . . . . . . . . . . . . . . . . . . 45 Christopher Lueg Applications The Fastap Keypad and Pervasive Computing

93

Contribution of unresolved point sources to the galactic diffuse emission  

E-Print Network [OSTI]

The detection by the HESS atmospheric Cherenkov telescope of fifteen new sources from the Galactic plane makes it possible to estimate the contribution of unresolved point sources like those detected by HESS to the diffuse Galactic emission measured by EGRET and recently at higher energies by the Milagro Collaboration. Assuming that HESS sources have all the same intrinsic luminosity, the contribution of this new source population can account for most of the Milagro $\\gamma$-ray emission at TeV energies and between 10 and 20 per cent of EGRET diffuse Galactic $\\gamma$-ray emission for energies bigger than 10 GeV. Also, by combining the HESS and the Milagro results, constraints can be put on the distribution and the luminosities of gamma ray emitters in the Galaxy.

Sabrina Casanova; Brenda L. Dingus

2006-09-12T23:59:59.000Z

94

VIBRATION->VIBRATION ENERGY TRANSFER IN METHANE  

E-Print Network [OSTI]

VIBRATION ENERGY TRANSFER IN METHANE Peter Hess, A. H. Kung,Rotation Spectra of Methane, U.S. Nat'L· Tech. Inform.tret t tllll. I. INTRODUCTION Methane is a relatively simple

Hess, Peter

2012-01-01T23:59:59.000Z

95

Rock art boundaries: considering geographically limited elements within the Pecos River Style  

E-Print Network [OSTI]

Dering, Jim Finnegan, Tommy Grey, Hubert Gubbels, Jim Bob Hargrove, Jack and Missy Harrington, Jerome Hesse, Howard Hunt, Roy Hurley, John and Judy Krevling, Lonnie Lischka, Ken Moore, Steve Norman, Elton Prewitt, Clyde Pursley, Rick Rylander, Rod Sanders...

Harrison, James Burr

2004-09-30T23:59:59.000Z

96

Diffuse TeV Emission at the Galactic Centre  

E-Print Network [OSTI]

The High-Energy Stereoscopic System (HESS) has detected intense diffuse TeV emission correlated with the distribution of molecular gas along the galactic ridge at the centre of our Galaxy. Earlier HESS observations of this region had already revealed the presence of several point sources at these energies, one of them (HESS J1745-290) coincident with the supermassive black hole Sagittarius A*. It is still not entirely clear what the origin of the TeV emission is, nor even whether it is due to hadronic or leptonic interactions. It is reasonable to suppose, however, that at least for the diffuse emission, the tight correlation of the intensity distribution with the molecular gas indicates a pionic-decay process involving relativistic protons. In this paper, we explore the possible source(s) of energetic hadrons at the galactic centre, and their propagation through a turbulent medium. We conclude that though Sagittarius A* itself may be the source of cosmic rays producing the emission in HESS J1745-290, it cannot be responsible for the diffuse emission farther out. A distribution of point sources, such as pulsar wind nebulae dispersed along the galactic plane, similarly do not produce a TeV emission profile consistent with the HESS map. We conclude that only a relativistic proton distribution accelerated throughout the inter-cloud medium can account for the TeV emission profile measured with HESS.

Elizabeth Wommer; Fulvio Melia; Marco Fatuzzo

2008-04-18T23:59:59.000Z

97

Title of dissertation: CONTROL, DYNAMICS, AND EPIDEMIC SPREADING IN COMPLEX SYSTEMS  

E-Print Network [OSTI]

To my wife Zsofi and to my parents ii #12;Acknowledgments There are many people to whom I am grateful scientific ideas are lost if not conveyed in a clear accessible manner. He is he sharpest minded critic and professionalism of Jane Hessing. Finally, I would like to thank my parents for their encouragement and support. iv

Anlage, Steven

98

Short Communication Effect of exogenous electron shuttles on growth and fermentative metabolism  

E-Print Network [OSTI]

Research Centre, Kalpakkam 603102, Tamil Nadu, India c Division of Advanced Nuclear Engineering, POSTECH of ESs can cre- ate alternate electron flows, thereby affecting the fermentation pattern and biofuel are of special interest in biofuel production from lignocellu- losic biomass (Hess et al., 2011) due

Johnson, Peter D.

99

What to Do When Your Hessian Is Not Invertible  

E-Print Network [OSTI]

What to Do When Your Hessian Is Not Invertible Alternatives to Model Respecification in Nonlinear is not invertable? The standard textbook advice is to respecify the model, but this is another way of saying for its inventor, German mathematician Ludwig Hesse) must be positive definite and hence invertible

Gill, Jeff

100

Original article Soil CO2 efflux in a beech forest: dependence on soil  

E-Print Network [OSTI]

Original article Soil CO2 efflux in a beech forest: dependence on soil temperature and soil water 1998) Abstract - Our objective was to quantify the annual soil carbon efflux in a young beech forest in north-eastern France (Hesse Forest, Euroflux site FR02) from measurements of soil CO, efflux. Soil CO

Paris-Sud XI, Université de

Note: This page contains sample records for the topic "amerada hess hess" 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

Your Career as Alumni Student Careers Forum  

E-Print Network [OSTI]

Anode Plant Oak Ridge Reservation Bulgarian Wireless Network Khursaniyah Gas Plant Jamnagar Refinery Mountain Repository Refinery KG D6 Gas Development Thai Oil Paraxylene 4G Communications High Speed 1Hess Gas Development Motiva Refinery Yarwun 2 Refinery #12;10/23/2008 4 Rock Anchoring A di P j t Alumni

Militzer, Burkhard

102

New Technology@Home: Impacts on Usage Behavior and Social Structures  

E-Print Network [OSTI]

New Technology@Home: Impacts on Usage Behavior and Social Structures Jan Hess, Benedikt Ley.wulf}@uni-siegen.de ABSTRACT Studying domestic usage contexts has become an important field in research. Recent technological. The adoption and appropriation of new devices and technologies has led to a more flexible usage behavior

103

Special Issue: "Thinking beyond the Box: Designing Interactive TV across Different Devices"  

E-Print Network [OSTI]

provides new opportunities for using home-related services including online gaming, visualization of energy" Behavior & Information Technology (BIT) Guest Editors: Jan Hess, Hendrik Knoche, Volker Wulf Nowadays consumption, home security or support for healthy living. The TV set is thus becoming a high-tech platform

104

Generalising the GHS Attack on the Elliptic Curve Discrete Logarithm Problem  

E-Print Network [OSTI]

Generalising the GHS Attack on the Elliptic Curve Discrete Logarithm Problem F. Hess Technical succumb to the basic GHS attack, thereby weakening curves over F2155 further. We also discuss other possible extensions or variations of the GHS attack and conclude that they are not likely to yield further

Hess, Florian

105

The GHS Attack Revisited Computer Science Department,  

E-Print Network [OSTI]

The GHS Attack Revisited F. Hess Computer Science Department, Woodland Road, University of Bristol the number of elliptic curves which succumb to the basic GHS attack, thereby weakening curves over F2155 further. We also discuss other possible extensions or variations of the GHS attack and conclude

Hess, Florian

106

Extending the GHS Weil Descent Attack No Author Given  

E-Print Network [OSTI]

Extending the GHS Weil Descent Attack No Author Given No Institute Given Abstract. In this paper we extend the Weil descent attack due to Gaudry, Hess and Smart (GHS) to a much larger class of elliptic curves. This extended attack applies to elds of composite degree over F2 . The principle behind

Hess, Florian

107

Analysis of the GHS Weil Descent Attack on the ECDLP over Characteristic Two Finite Fields of Composite Degree  

E-Print Network [OSTI]

Analysis of the GHS Weil Descent Attack on the ECDLP over Characteristic Two Finite Fields, we analyze the Gaudry-Hess-Smart (GHS) Weil descent attack on the elliptic curve discrete logarithm with these parameters; and (ii) the GHS attack is more eÃ?cient for solving the ECDLP in E(F 2 N ) than for solving

Teske, Edlyn

108

Free loop spaces in topology and  

E-Print Network [OSTI]

Free loop spaces in topology and physics Kathryn Hess What is the space of free loops? Enumeration of geodesics Hochschild and cyclic homology Homological conformal field theories Free loop spaces in topology Meeting of the Edinburgh Mathematical Society Glasgow, 14 November 2008 #12;Free loop spaces in topology

Thévenaz, Jacques

109

Snake River Fall Chinook Salmon Productivity Nez Perce Tribe  

E-Print Network [OSTI]

Snake River Fall Chinook Salmon Productivity Jay Hesse Nez Perce Tribe Department of Fisheries salmon abundance and productivity have been and continue to be influenced by construction and operation related to productivity; (1) adult abundance, (2) hatchery programs, (3) management actions, and (4

110

Hydrol. Earth Syst. Sci., 15, 519532, 2011 www.hydrol-earth-syst-sci.net/15/519/2011/  

E-Print Network [OSTI]

Reliability and robustness of rainfall compound distribution model based on weather pattern sub-sampling F of shape parameter; (iii) the MEWP distribution proved to be robust and reliable, demon- strating.5194/hess-15-519-2011 © Author(s) 2011. CC Attribution 3.0 License. Hydrology and Earth System Sciences

Paris-Sud XI, Université de

111

THE ECONOMIC SITUATION IN THE ECE REGION  

E-Print Network [OSTI]

THE ECONOMIC SITUATION IN THE ECE REGION DIETER HESSE ECONOMIC ANALYSIS DIVISION UNECE #12;Major trends in the global economy so far in 2003 Global economic activity picked up ­ but uneven regional growth forces United States remains main engine of global economic growth Japan and Asian emerging

112

Board of Trustees (Idaho State Board of Education)  

E-Print Network [OSTI]

and Environmental Health -School of Nursing -Radiologic Sciences -Respiratory Care -Research Assistance -Library Ventures -Research Compliance -CAES Energy Policy Institute -Story Initiative -CAES Energy Efficiency Newcomb Athletics*¨ Mark Coyle Internal Audit Larry Harmon Boise State Radio John Hess Morrison Center

Barrash, Warren

113

GCCC Students Hit the Road for the Summer Summer is around the corner, and GCCC students are taking advantage of the  

E-Print Network [OSTI]

-monitoring networks above CO2-EOR sites. Ph.D. student K-Won Chang is heading much farther east than Houston. He plans of the CO2 plume at Cranfield using seismic surveys. This summer she's off to Houston, where she Development Group. Also headed to Houston, Marlo Gawey will be working on an EOR project with Hess Corporation

Texas at Austin, University of

114

Particle Size Distribution of Gypseous Samples  

E-Print Network [OSTI]

to conditions in the field. In order to understand the true characterization of the soil and the gypsum particles, the entire soil sample should be analyzed. Four different approaches to the BaCl2 method presented in the literature (Hesse, 1976, Matar...

Arnett, Morgan P.

2010-01-16T23:59:59.000Z

115

Weston Buckley Anderson Department of Earth and Environmental Science  

E-Print Network [OSTI]

-2893-2012. Anderson, W.B., Guikema S., Zaitchik, B. and Pan, W. (2014): Methods for estimating population density University Research: Characterized the 2010-11 East Africa drought using remote sensing products Advisor: Dr drought monitor for East Africa, Hydrol. Earth Syst. Sci., 16, 2893-2913, doi:10.5194/hess-16

116

The Astrophysical Multimessenger Observatory Network (AMON) M.W.E. Smith a,b,  

E-Print Network [OSTI]

Gravitational radiation Neutrinos Cosmic rays Gamma-ray bursts Supernovae a b s t r a c t We summarize including the Swift [6] and Fermi [7] satellites, the HESS [8], VERITAS [9], and MAGIC [10] TeV gamma-ray telescopes, and the HAWC [11] TeV gamma-ray observatory. Collectively, these facilities promise the first

Babu, G. Jogesh

117

SEMINAR SERIES Towards a climate sensitive  

E-Print Network [OSTI]

in an Earth System Model presented by Peter Hess Associate Professor, Biological and Environmental Engineering are crudely represented in Earth System Models and do not respond changes in climate. Here I present a first interactive parameterization of ammonia emissions in an Earth System Model based on model physics and discuss

118

Physical mapping and characterization of the equine lymphocyte antigen (ELA) complex  

E-Print Network [OSTI]

. 1990) in addition to the LMP2, LMP7, TAP1, TAP2, DOB, and DOA which are present in the class II regions of all mammalian MHCs studied to date (Hess et al. 1999). Comparative sequence analysis of DYA and DIB exons has not identified any orthologous...

Seabury, Ashley Gustafson

2005-08-29T23:59:59.000Z

119

ICRC 2007: Mrida, Mexico Highlights from the Pierre Auger Observatory  

E-Print Network [OSTI]

and side-by- side." V.H.Hess, Nobel Lecture, December 1936 #12;2 Argentina Australia Brasil Bolivia* Mexico (stereo ­ low N) ~ 0.2° ~ 1 - 2° ~ 3 - 5° Flat with energy AND E, A, spectral mass and model (M) free slope and M dependent A and M free A and M A and M free dependent Angular Resolution Aperture Energy #12

120

Status of Identification of VHE Gamma-Ray Sources  

SciTech Connect (OSTI)

With the recent advances made by Cherenkov telescopes such as H.E.S.S. the field of very high-energy (VHE) {gamma}-ray astronomy has recently entered a new era in which for the first time populations of Galactic sources such as e.g. Pulsar wind nebulae (PWNe) or Supernova remnants (SNRs) can be studied. However, while some of the new sources can be associated by positional coincidence as well as by consistent multi-wavelength data to a known counterpart at other wavelengths, most of the sources remain not finally identified. In the following, the population of Galactic H.E.S.S. sources will be used to demonstrate the status of the identifications, to classify them into categories according to this status and to point out outstanding problems.

Funk, Stefan; /SLAC

2006-09-28T23:59:59.000Z

Note: This page contains sample records for the topic "amerada hess hess" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
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We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


121

Hybrid model of GeV-TeV gamma ray emission from Galactic Center  

E-Print Network [OSTI]

The observations of high energy $\\gamma$-ray emission from the Galactic center (GC) by HESS, and recently by Fermi, suggest the cosmic ray acceleration in the GC and possibly around the supermassive black hole. In this work we propose a lepton-hadron hybrid model to explain simultaneously the GeV-TeV $\\gamma$-ray emission. Both electrons and hadronic cosmic rays were accelerated during the past activity of the GC. Then these particles would diffuse outwards and interact with the interstellar gas and background radiation field. The collisions between hadronic cosmic rays with gas is responsible to the TeV $\\gamma$-ray emission detected by HESS. With fast cooling in the strong radiation field, the electrons would cool down and radiate GeV photons through inverse Compton scattering off the soft background photons. This scenario provides a natural explanation of the observed GeV-TeV spectral shape of $\\gamma$-rays.

Yi-Qing Guo; Qiang Yuan; Cheng Liu; Ai-Feng Li

2014-09-14T23:59:59.000Z

122

Multiwavelength campaign on the HBL PKS~2155-304 : A new insight on its spectral energy distribution  

E-Print Network [OSTI]

The blazar PKS~2155-304 was the target of a multiwavelength campaign from June to October 2013 which widely improves our knowledge of its spectral energy distribution. This campaign involved the NuSTAR satellite (3-79 keV), the Fermi Large Area Telescope (LAT, 100~MeV-300~GeV) and the High Energy Stereoscopic System (H.E.S.S.) array phase II (with an energy threshold of few tens of GeV). While the observations with NuSTAR extend the X-ray spectrum to higher energies than before, H.E.S.S. phase II, together with the use of the LAT PASS 8, enhance the coverage of the $\\gamma$-ray regime with an unprecedented precision. In this work, preliminary results from the multi-wavelength analysis are presented.

Sanchez, D A; Zaborov, D; Parson, D; Madejski, G M; NuSTAR, A Furniss On behalf of the; Fermi,

2015-01-01T23:59:59.000Z

123

Steam Partnerships: Case Study of Improved Energy Efficiency  

E-Print Network [OSTI]

Steam Partnerships: Case Study of Improved Energy Efficiency Michael V. Calogero, P.E., CEM Robert E. Hess Novi Leigh Director, Northeast Operations Sr. Energy Systems Engineer Energy Systems Engineer Armstrong Service, Inc ABSTRACT Effective.... 1998-2001 operating data from client's laundry processing facility. 3. Turner, Wayne C., Energy Management Handbook, 2 nd edition, 1993. 4. Armstrong International, Inc., Steam Conservation Guidelines for Condensate Drainage, Handbook N-1 01, 1997...

Calogero, M. V.; Hess, R. E.; Leigh, N.

124

The development and operational testing of an experimental reactor for gas-liquid-solid reaction systems at high temperatures and pressures  

E-Print Network [OSTI]

shaft. With the impeller in place and rotating, gas was drawn into the top port and ejected at the impeller mount. The reactor pressure was monitored via the transducer port. The transducer was a Viatran Pressure Transducer, model 103. The liquid...THE DEVELOPMENT AND OPERATIONAL TESTING OF AN EXPERIMENTAL REACTOR FOR GAS-LIQUID-SOLID REACTION SYSTEMS AT HIGH TEMPERATURES AND PRESSURES A Thesis by RICHARD KENNETH HESS Submitted to the Graduate College of Texas A&M University in partial...

Hess, Richard Kenneth

2012-06-07T23:59:59.000Z

125

Gamma-ray and neutrino fluxes from Heavy Dark Matter in the Galactic Center  

E-Print Network [OSTI]

We present a study of the Galactic Center region as a possible source of both secondary gamma-ray and neutrino fluxes from annihilating dark matter. We have studied the gamma-ray flux observed by the High Energy Stereoscopic System (HESS) from the J1745-290 Galactic Center source. The data are well fitted as annihilating dark matter in combination with an astrophysical background. The analysis was performed by means of simulated gamma spectra produced by Monte Carlo event generators packages. We analyze the differences in the spectra obtained by the various Monte Carlo codes developed so far in particle physics. We show that, within some uncertainty, the HESS data can be fitted as a signal from a heavy dark matter density distribution peaked at the Galactic Center, with a power-law for the background with a spectral index which is compatible with the Fermi-Large Area Telescope (LAT) data from the same region. If this kind of dark matter distribution generates the gamma-ray flux observed by HESS, we also expect to observe a neutrino flux. We show prospective results for the observation of secondary neutrinos with the Astronomy with a Neutrino Telescope and Abyss environmental RESearch project (ANTARES), Ice Cube Neutrino Observatory (Ice Cube) and the Cubic Kilometer Neutrino Telescope (KM3NeT). Prospects solely depend on the device resolution angle when its effective area and the minimum energy threshold are fixed.

V. Gammaldi; J. A. R. Cembranos; A. de la Cruz-Dombriz; R. A. Lineros; A. L. Maroto

2014-04-09T23:59:59.000Z

126

The Cosmic Ray Distribution in Sagittarius B  

E-Print Network [OSTI]

The HESS instrument has observed a diffuse flux of ~ TeV gamma rays from a large solid angle around the Galactic center (GC). This emission is correlated with the distribution of gas in the region suggesting that the gamma rays originate in collisions between cosmic ray hadrons (CRHs) and ambient matter. Of particular interest, HESS has detected gamma rays from the Sagittarius (Sgr) B Molecular Cloud Complex. Prompted by the suggestion of a hadronic origin for the gamma rays, we have examined archival 330 and 74 MHz Very Large Array radio data and 843 MHz Sydney University Molonglo Sky Survey data covering Sgr B, looking for synchrotron emission from secondary electrons and positrons (expected to be created in the same interactions that supply the observed gamma rays). Intriguingly, we have uncovered non-thermal emission, but at a level exceeding expectation. Adding to the overall picture, recent observations by the Atacama Pathfinder Experiment telescope show that the cosmic ray ionization rate is ten times greater in the Sgr B2 region of Sgr B than the local value. Lastly, Sgr B2 is also a very bright X-ray source. We examine scenarios for the spectra of CRHs and/or primary electrons that would reconcile all these different data. We determine that (i) a hard (~ E^-2.2), high-energy (> TeV) population CRHs is unavoidably required by the HESS gamma ray data and (ii) the remaining broad-band, non-thermal phenomenology is explained either by a rather steep (~ E^-2.9) spectrum of primary electrons or a (~ E^-2.7) population of CRHs. No single, power-law population of either leptons or hadrons can explain the totality of broadband, non-thermal Sgr B phenomenology.

Roland M. Crocker; David Jones; Raymond J. Protheroe; Juergen Ott; Ron Ekers; Fulvio Melia; Todor Stanev; Anne Green

2007-03-23T23:59:59.000Z

127

Dark matter annihilation and the PAMELA, FERMI, and ATIC anomalies  

SciTech Connect (OSTI)

If dark matter annihilation accounts for the tantalizing excess of cosmic ray electron/positrons, as reported by the PAMELA, ATIC, HESS, and FERMI observatories, then the implied annihilation cross section must be relatively large. This results, in the context of standard cosmological models, in very small relic dark matter abundances that are incompatible with astrophysical observations. We explore possible resolutions to this apparent conflict in terms of nonstandard cosmological scenarios; plausibly allowing for large cross sections, while maintaining relic abundances in accord with current observations.

El Zant, A. A.; Okada, H. [Centre for Theoretical Physics, British University in Egypt, El Sherouk City, Postal No, 11837, Post Office Box 43 (Egypt); Khalil, S. [Centre for Theoretical Physics, British University in Egypt, El Sherouk City, Postal No, 11837, Post Office Box 43 (Egypt); Department of Mathematics, Ain Shams University, Faculty of Science, Cairo, 11566 (Egypt)

2010-06-15T23:59:59.000Z

128

Pulsar model of the high energy phenomenology of LS 5039  

E-Print Network [OSTI]

Under the assumption that LS 5039 is a system composed by a pulsar rotating around an O6.5V star in a $\\sim 3.9$ day orbit, we present the results of a theoretical modeling of the high energy phenomenology observed by the High Energy Stereoscopy Array (H.E.S.S.). This model (including detailed account of the system geometry, Klein-Nishina inverse Compton, $\\gamma$-$\\gamma$ absorption, and cascading) is able to describe well the rich observed phenomenology found in the system at all timescales, both flux and spectrum-wise.

Agnieszka Sierpowska-Bartosik; Diego F. Torres

2007-10-04T23:59:59.000Z

129

Dark matter conversion as a source of boost factor for explaining the cosmic ray positron and electron excesses  

E-Print Network [OSTI]

In interacting multi-component dark matter (DM) models, if the DM components are nearly degenerate in mass and the interactions between them are strong enough, the relatively heavy DM components can be converted into lighter ones at late time after the thermal decoupling. Consequently, the relic density of the lightest DM component can be considerably enhanced at late time. This may contribute to an alternative source of boost factor required to explain the positron and electron excesses reported by the recent DM indirect search experiments such as PAMELA, Fermi-LAT and HESS etc..

Ze-Peng Liu; Yue-Liang Wu; Yu-Feng Zhou

2011-12-17T23:59:59.000Z

130

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

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsruc DocumentationP-SeriesFlickr FlickrGuidedCH2M HILL SecretaryHazmatHelping Those inHenryHess

131

Nancy Mitman  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsrucLas Conchas recoveryLaboratory | NationalJohn F. Geisz,AerialStaff NUG 2012NakayasuJ. Hess

132

Nancy Washton | EMSL  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsrucLas Conchas recoveryLaboratory | NationalJohn F. Geisz,AerialStaff NUG 2012NakayasuJ. HessWashton

133

The dual axis radiographic hydrodynamic test (DARHT) facility personnel safety system (PSS) control system  

SciTech Connect (OSTI)

The mission of the Dual Axis Radiograph Hydrodynamic Test (DARHT) Facility is to conduct experiments on dynamic events of extremely dense materials. The PSS control system is designed specifically to prevent personnel from becoming exposed to radiation and explosive hazards during machine operations and/or the firing site operation. This paper will outline the Radiation Safety System (RSS) and the High Explosive Safety System (HESS) which are computer-controlled sets of positive interlocks, warning devices, and other exclusion mechanisms that together form the PSS.

Jacquez, Edward B [Los Alamos National Laboratory

2008-01-01T23:59:59.000Z

134

10 Years after the 2003 Northeast Blackout | Department of Energy  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "of EnergyEnergyENERGYWomenthe House Committee onsupports high impactSinceDr.2,Nancy Hess | Photo Courtesy

135

103323_DOE-IE L48 workshops flier r3.indd  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "of EnergyEnergyENERGYWomenthe House Committee onsupports high impactSinceDr.2,Nancy Hess |

136

Dynamic pressure response of water flow between closely spaced roughened flat plates  

E-Print Network [OSTI]

of MASTER OF SCIENCE May 1993 Major Subject: Mechanical Engineering DYNAMIC PRESSURE RESPONSE OF WATER FLOW BETWEEN CLOSELY SPACED ROUGHENED FLAT PLATES A Thesis by JOHN CHARLES HESS Approved as to style and content by: Robert E. DeOtte, Jr. (Co.... S. , Texas A&M University Co-Chairs of Advisory Committee: Dr. R. E. DeOtte, Jr, Dr. G, L, Morrison A flat plate tester was designed and built to determine friction factors and dynamic pressures for water flow over smooth, knurl, and cavity...

Hess, John Charles

2012-06-07T23:59:59.000Z

137

Neutrinos from the Galactic Center in the Light of its Gamma-Ray Detection at TeV Energy  

E-Print Network [OSTI]

We re-evaluate the event rate expected in km^3-scale detectors for neutrinos from the direction of the Galactic Center (GC) in light of recent spectral measurements obtained by the HESS instrument for ~TeV gamma-radiation from this direction. In the most plausible scenario the re-evaluated event rate is smaller than that previously calculated--and here re-calculated--on the basis of EGRET data. However, the GC TeV gamma-ray detections by the Whipple, CANGAROO, and HESS instruments, together with the strong indications for an overabundance of cosmic rays coming from the GC at EeV energies, strengthen the expectation for a detectable, TeV-PeV GC neutrino signal from proton-proton interactions in that region. If the TeV gamma-ray--EeV cosmic ray anisotropy connection is correct, this signal will be detectable within a year and half for km^3-scale neutrino detectors in the Northern Hemisphere at super-TeV energies and, significantly, should also be detectable in 1.6 years by the South Polar IceCube detector at energies > 10^14 eV. The GC neutrino signal should also produce a detectable signal from neutrino showering and resonant W^- production by anti-electron-neutrinos in the volume of a km^3-scale detector.

Roland M. Crocker; Fulvio Melia; Raymond R. Volkas

2005-02-10T23:59:59.000Z

138

Simultaneous multi-wavelength campaign on PKS 2005-489 in a high state  

E-Print Network [OSTI]

The high-frequency peaked BL Lac object PKS 2005-489 was the target of a multi-wavelength campaign with simultaneous observations in the TeV gamma-ray (H.E.S.S.), GeV gamma-ray (Fermi/LAT), X-ray (RXTE, Swift), UV (Swift) and optical (ATOM, Swift) bands. This campaign was carried out during a high flux state in the synchrotron regime. The flux in the optical and X-ray bands reached the level of the historical maxima. The hard GeV spectrum observed with Fermi/LAT connects well to the very high energy (VHE, E>100GeV) spectrum measured with H.E.S.S. with a peak energy between ~5 and 500 GeV. Compared to observations with contemporaneous coverage in the VHE and X-ray bands in 2004, the X-ray flux was ~50 times higher during the 2009 campaign while the TeV gamma-ray flux shows marginal variation over the years. The spectral energy distribution during this multi-wavelength campaign was fit by a one zone synchrotron self-Compton model with a well determined cutoff in X-rays. The parameters of a one zone SSC model ar...

Abramowski, A; Aharonian, F; Akhperjanian, A G; Anton, G; Barnacka, A; de Almeida, U Barres; Bazer-Bachi, A R; Becherini, Y; Becker, J; Behera, B; Bernlöhr, K; Bochow, A; Boisson, C; Bolmont, J; Bordas, P; Borrel, V; Brucker, J; Brun, F; Brun, P; Bulik, T; Büsching, I; Casanova, S; Cerruti, M; Chadwick, P M; Charbonnier, A; Chaves, R C G; Cheesebrough, A; Chounet, L -M; Clapson, A C; Coignet, G; Conrad, J; Dalton, M; Daniel, M K; Davids, I D; Degrange, B; Deil, C; Dickinson, H J; Djannati-Ataï, A; Domainko, W; Drury, L O'C; Dubois, F; Dubus, G; Dyks, J; Dyrda, M; Egberts, K; Eger, P; Espigat, P; Fallon, L; Farnier, C; Fegan, S; Feinstein, F; Fernandes, M V; Fiasson, A; Fontaine, G; Förster, A; Füßling, M; Gabici, S; Gallant, Y A; Gast, H; Gérard, L; Gerbig, D; Giebels, B; Glicenstein, J F; Glück, B; Goret, P; Göring, D; Hague, J D; Hampf, D; Hauser, M; Heinz, S; Heinzelmann, G; Henri, G; Hermann, G; Hinton, J A; Hoffmann, A; Hofmann, W; Hofverberg, P; Horns, D; Jacholkowska, A; de Jager, O C; Jahn, C; Jamrozy, M; Jung, I; Kastendieck, M A; Katarzy?ski, K; Katz, U; Kaufmann, S; Keogh, D; Kerschhaggl, M; Khangulyan, D; Khélifi, B; Klochkov, D; Klu?niak, W; Kneiske, T; Komin, Nu; Kosack, K; Kossakowski, R; Laffon, H; Lamanna, G; Lenain, J -P; Lennarz, D; Lohse, T; Lopatin, A; Lu, C -C; Marandon, V; Marcowith, A; Masbou, J; Maurin, D; Maxted, N; McComb, T J L; Medina, M C; Méhault, J; Nguyen, N; Moderski, R; Moulin, E; Naumann-Godo, M; de Naurois, M; Nedbal, D; Nekrassov, D; Nicholas, B; Niemiec, J; Nolan, S J; Ohm, S; Olive, J-F; Wilhelmi, E de Oña; Opitz, B; Ostrowski, M; Panter, M; Arribas, M Paz; Pedaletti, G; Pelletier, G; Petrucci, P -O; Pita, S; Pühlhofer, G; Punch, M; Quirrenbach, A; Raue, M; Rayner, S M; Reimer, A; Reimer, O; Renaud, M; Reyes, R de los; Rieger, F; Ripken, J; Rob, L; Rosier-Lees, S; Rowell, G; Rudak, B; Rulten, C B; Ruppel, J; Ryde, F; Sahakian, V; Santangelo, A; Schlickeiser, R; Schöck, F M; Schönwald, A; Schwanke, U; Schwarzburg, S; Schwemmer, S; Shalchi, A; Sikora, M; Skilton, J L; Sol, H; Spengler, G; Stawarz, ?; Steenkamp, R; Stegmann, C; Stinzing, F; Sushch, I; Szostek, A; Tam, P H; Tavernet, J -P; Terrier, R; Tibolla, O; Tluczykont, M; Valerius, K; van Eldik, C; Vasileiadis, G; Venter, C; Vialle, J P; Viana, A; Vincent, P; Vivier, M; Völk, H J; Volpe, F; Vorobiov, S; Vorster, M; Wagner, S J; Ward, M; Wierzcholska, A; Zajczyk, A; Zdziarski, A A; Zech, A; Zechlin, H -S; Abdo, A A; Ackermann, M; Ajello, M; Baldini, L; Ballet, J; Barbiellini, G; Bastieri, D; Bechtol, K; Bellazzini, R; Berenji, B; Blandford, R D; Bonamente, E; Borgland, A W; Bregeon, J; Brez, A; Brigida, M; Bruel, P; Buehler, R; Buson, S; Caliandro, G A; Cameron, R A; Cannon, A; Caraveo, P A; Carrigan, S; Casandjian, J M; Cavazzuti, E; Cecchi, C; Çelik, Ö; Chekhtman, A; Cheung, C C; Chiang, J; Ciprini, S; Claus, R; Cohen-Tanugi, J; Cutini, S; Dermer, C D; de Palma, F; Silva, E do Couto e; Drell, P S; Dubois, R; Dumora, D; Escande, L; Favuzzi, C; Ferrara, E C; Focke, W B; Fortin, P; Frailis, M; Fukazawa, Y; Fusco, P; Gargano, F; Gasparrini, D; Gehrels, N; Germani, S; Giglietto, N; Giommi, P; Giordano, F; Giroletti, M; Glanzman, T; Godfrey, G; Grenier, I A; Grove, J E; Guiriec, S; Hadasch, D; Hays, E; Horan, D; Hughes, R E; Jóhannesson, G; Johnson, A S; Johnson, W N; Kamae, T; Katagiri, H; Kataoka, J; Knödlseder, J; Kuss, M; Lande, J; Latronico, L; Lee, S -H; Longo, F; Loparco, F; Lott, B; Lovellette, M N; Lubrano, P; Madejski, G M; Makeev, A; Mazziotta, M N; McConville, W; McEnery, J E; Michelson, P F; Mizuno, T; Monte, C; Monzani, M E; Morselli, A; Moskalenko, I V; Murgia, S; Nakamori, T; Nishino, S; Nolan, P L; Norris, J P; Nuss, E; Ohsugi, T; Okumura, A; Omodei, N; Orlando, E; Ormes, J F; Ozaki, M; Paneque, D; Panetta, J H; Parent, D; Pelassa, V; Pepe, M; Pesce-Rollins, M; Piron, F; Porter, T A; Rainò, S; Rando, R; Razzano, M; Sadrozinski, H F -W; Sanchez, D; Sander, A; Sgrò, C; Siskind, E J; Smith, P D; Spandre, G; Spinelli, P; Strickman, M S; Suson, D J; Takahashi, H; Takahashi, T; Tanaka, T; Thayer, J B; Thayer, J G; Thompson, D J; Tibaldo, L; Torres, D F; Tosti, G; Tramacere, A; Troja, E; Uehara, T; Usher, T L; Vandenbroucke, J; Vianello, G; Vilchez, N; Vitale, V; Waite, A P; Wang, P; Winer, B L; Wood, K S; Yang, Z; Ylinen, T; Ziegler, M

2011-01-01T23:59:59.000Z

139

A Gamma-Ray Burst/Pulsar for Cosmic-Ray Positrons with a Dark Matter-like Spectrum  

E-Print Network [OSTI]

We propose that a nearby gamma-ray burst (GRB) or GRB-like (old, single and short-lived) pulsar/supernova remnant/microquasar about 10^{5-6} years ago may be responsible for the excesses of cosmic-ray positrons and electrons recently observed by the PAMELA, ATIC/PPB-BETS, Fermi and HESS experiments. We can reproduce the smooth Fermi/HESS spectra as well as the spiky ATIC/PPB-BETS spectra. The spectra have a sharp cutoff that is similar to the dark matter predictions, sometimes together with a line (not similar), since higher energy cosmic-rays cool faster where the cutoff/line energy marks the source age. A GRB-like astrophysical source is expected to have a small but finite spread in the cutoff/line as well as anisotropy in the cosmic-ray and diffuse gamma-ray flux, providing a method for the Fermi and future CALET experiments to discriminate between dark matter and astrophysical origins.

Kunihito Ioka

2010-06-15T23:59:59.000Z

140

Q-branch Raman scattering and modern kinetic thoery  

SciTech Connect (OSTI)

The program is an extension of previous APL work whose general aim was to calculate line shapes of nearly resonant isolated line transitions with solutions of a popular quantum kinetic equation-the Waldmann-Snider equation-using well known advanced solution techniques developed for the classical Boltzmann equation. The advanced techniques explored have been a BGK type approximation, which is termed the Generalized Hess Method (GHM), and conversion of the collision operator to a block diagonal matrix of symmetric collision kernels which then can be approximated by discrete ordinate methods. The latter method, which is termed the Collision Kernel method (CC), is capable of the highest accuracy and has been used quite successfully for Q-branch Raman scattering. The GHM method, not quite as accurate, is applicable over a wider range of pressures and has proven quite useful.

Monchick, L. [The Johns Hopkins Univ., Laurel, MD (United States)

1993-12-01T23:59:59.000Z

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141

GLAST and Ground-Based Gamma-Ray Astronomy  

SciTech Connect (OSTI)

The launch of the Gamma-ray Large Area Space Telescope (GLAST) in 2007 will open the possibility of combined studies of astrophysical sources with existing ground-based VHE {gamma}-ray experiments such as H.E.S.S., VERITAS and MAGIC. Ground-based {gamma}-ray observatories provide complementary capabilities for spectral, temporal, spatial and population studies of high-energy {gamma}-ray sources. Joint observations cover a huge energy range, from 20 MeV to over 50 TeV. The LAT will survey the entire sky every three hours, allowing us to perform long-term monitoring of variable sources under uniform observation conditions and to detect flaring sources promptly. Imaging atmospheric Cherenkov telescopes (IACTs) will complement these observations with high-sensitivity pointed observations on regions of interest.

Funk, S.; Carson, J.E.; Giebels, B.; Longo, F.; McEnery, J.E.; Paneque, D.; Reimer, O.; Reyes, L.C.

2007-10-10T23:59:59.000Z

142

The Spectral Break Near TeV of $e^\\pm$ Cosmic Rays - Standard Physics or Dark Matter Origin?  

E-Print Network [OSTI]

The complex spectra of high energy ${\\rm e^\\pm}$ cosmic rays (CRs) observed near Earth are those expected from standard model physics. In particular, the observed hardening of their spectra with increasing energy reported by the AMS-02 collaboration can be produced by the transition of their energy-loss by inverse Compton scattering off Galactic light from the Thomson to the Klein-Nishina regime. The "cut-off" near TeV in the combined ${\\rm e^\\pm}$ flux observed with H.E.S.S can be due to pair production in ${\\rm e^\\pm}\\gamma$ collisions in source rather than a bump produced by the decay/annihilation of dark matter particles with a mass of $\\sim$TeV. Beyond this "cutoff", the $e^\\pm$ CRs are mostly produced by the decay of mesons from hadronic collisions of CR protons in/near source with a positron fraction $\\sim 0.57$.

Dado, Shlomo

2015-01-01T23:59:59.000Z

143

TIMING AND INTERSTELLAR SCATTERING OF 35 DISTANT PULSARS DISCOVERED IN THE PALFA SURVEY  

SciTech Connect (OSTI)

We have made extensive observations of 35 distant slow (non-recycled) pulsars discovered in the ongoing Arecibo PALFA pulsar survey. Timing observations of these pulsars over several years at Arecibo Observatory and Jodrell Bank Observatory have yielded high-precision positions and measurements of rotation properties. Despite being a relatively distant population, these pulsars have properties that mirror those of the previously known pulsar population. Many of the sources exhibit timing noise, and one underwent a small glitch. We have used multifrequency data to measure the interstellar scattering properties of these pulsars. We find scattering to be higher than predicted along some lines of sight, particularly in the Cygnus region. Finally, we present XMM-Newton and Chandra observations of the youngest and most energetic of the pulsars, J1856+0245, which has previously been associated with the GeV-TeV pulsar wind nebula HESS J1857+026.

Nice, D. J. [Department of Physics, Lafayette College, Easton, PA 18042 (United States); Altiere, E.; Farrington, D.; Popa, L.; Wang, Y. [Department of Physics, Bryn Mawr College, Bryn Mawr, PA 19010 (United States); Bogdanov, S.; Camilo, F. [Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027 (United States); Cordes, J. M.; Brazier, A.; Chatterjee, S. [Astronomy Department, Cornell University, Ithaca, NY 14853 (United States); Hessels, J. W. T. [ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990-AA Dwingeloo (Netherlands); Kaspi, V. M. [Department of Physics, McGill University, Montreal, QC H3A 2T8 (Canada); Lyne, A. G.; Stappers, B. W. [Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Manchester M13 9PL (United Kingdom); Ransom, S. M. [NRAO, Charlottesville, VA 22903 (United States); Sanpa-arsa, S. [Department of Astronomy, University of Virginia, Charlottesville, VA 22903 (United States); Allen, B. [Max-Planck-Institut fuer Gravitationsphysik, D-30167 Hannover (Germany); Bhat, N. D. R. [Center for Astrophysics and Supercomputing, Swinburne University, Hawthorn, Victoria 3122 (Australia); Champion, D. J. [Max-Planck-Institut fuer Radioastronomie, D-53121 Bonn (Germany); Crawford, F. [Department of Physics and Astronomy, Franklin and Marshall College, Lancaster, PA 17604-3003 (United States); and others

2013-07-20T23:59:59.000Z

144

Belowground Carbon Cycling Processes at the Molecular Scale: An EMSL Science Theme Advisory Panel Workshop  

SciTech Connect (OSTI)

As part of the Belowground Carbon Cycling Processes at the Molecular Scale workshop, an EMSL Science Theme Advisory Panel meeting held in February 2013, attendees discussed critical biogeochemical processes that regulate carbon cycling in soil. The meeting attendees determined that as a national scientific user facility, EMSL can provide the tools and expertise needed to elucidate the molecular foundation that underlies mechanistic descriptions of biogeochemical processes that control carbon allocation and fluxes at the terrestrial/atmospheric interface in landscape and regional climate models. Consequently, the workshop's goal was to identify the science gaps that hinder either development of mechanistic description of critical processes or their accurate representation in climate models. In part, this report offers recommendations for future EMSL activities in this research area. The workshop was co-chaired by Dr. Nancy Hess (EMSL) and Dr. Gordon Brown (Stanford University).

Hess, Nancy J.; Brown, Gordon E.; Plata, Charity

2014-02-21T23:59:59.000Z

145

Collimation and Radiative Deceleration of Jets in TeV AGNs  

E-Print Network [OSTI]

We consider some implications of the rapid X-ray and TeV variability observed in M87 and the TeV blazars. We outline a model for jet focusing and demonstrate that modest radiative cooling can lead to recollimation of a relativistic jet in a nozzle having a very small cross-sectional radius. Such a configuration can produce rapid variability at large distances from the central engine and may explain recent observations of the HST-1 knot in M87. Possible applications of this model to TeV blazars are discussed. We also discuss a scenario for the very rapid TeV flares observed with HESS and MAGIC in some blazars, that accommodates the relatively small Doppler factors inferred from radio observations.

Amir Levinson; Omer Bromberg

2007-12-17T23:59:59.000Z

146

A Numerical Assessment of Cosmic-ray Energy Diffusion through Turbulent Media  

E-Print Network [OSTI]

How and where cosmic rays are produced, and how they diffuse through various turbulent media, represent fundamental problems in astrophysics with far reaching implications, both in terms of our theoretical understanding of high-energy processes in the Milky Way and beyond, and the successful interpretation of space-based and ground based GeV and TeV observations. For example, recent and ongoing detections, e.g., by Fermi (in space) and HESS (in Namibia), of $\\gamma$-rays produced in regions of dense molecular gas hold important clues for both processes. In this paper, we carry out a comprehensive numerical investigation of relativistic particle acceleration and transport through turbulent magnetized environments in order to derive broadly useful scaling laws for the energy diffusion coefficients.

Fatuzzo, Marco

2014-01-01T23:59:59.000Z

147

Simulation of Imaging Atmospheric Cherenkov Telescopes with CORSIKA and sim_telarray  

E-Print Network [OSTI]

Imaging Atmospheric Cherenkov Telescopes (IACTs) have resulted in a breakthrough in very-high energy (VHE) gamma-ray astrophysics. While early IACT installations faced the problem of detecting any sources at all, current instruments are able to see many sources, often over more than two orders of magnitude in energy. As instruments and analysis methods have matured, the requirements for calibration and modelling of physical and instrumental effects have increased. In this article, a set of Monte Carlo simulation tools is described that attempts to include all relevant effects for IACTs in great detail but aims to achieve this in an efficient and flexible way. These tools were originally developed for the HEGRA IACT system and later adapted for the H.E.S.S. experiment. Their inherent flexibility to describe quite arbitrary IACT systems makes them also an ideal tool for evaluating the potential of future installations. It is in use for design studies of CTA and other projects.

Konrad Bernlohr

2008-08-16T23:59:59.000Z

148

Phenomenology of Gamma-Ray Jets  

E-Print Network [OSTI]

We discuss some phenomenological aspects of $\\gamma$-ray emitting jets. In particular, we present calculations of the $\\gamma$-sphere and $\\pi$-sphere for various target photon fields, and employ them to demonstrate how $\\gamma$-ray observations at very high energies can be used to constraint the Doppler factor of the emitting plasma and the production of VHE neutrinos. We also consider the implications of the rapid TeV variability observed in M87 and the TeV blazars, and propose a model for the very rapid TeV flares observed with HESS and MAGIC in some blazars,that accommodates the relatively small Doppler factors inferred from radio observations. Finally, we briefly discuss the prospects for detecting VHE neutrinos from relativistic jets.

Amir Levinson

2007-09-10T23:59:59.000Z

149

Intergalactic Photon Spectra from the Far IR to the UV Lyman Limit for $0 Optical Depth of the Universe to High Energy Gamma-Rays  

E-Print Network [OSTI]

We calculate the intergalactic photon density as a function of both energy and redshift for 0 gamma-rays in intergalactic space owing to interactions with low energy photons and the 2.7 K cosmic background radiation. We calculate the optical depth of the universe, tau, for gamma-rays having energies from 4 GeV to 100 TeV emitted by sources at redshifts from ~0 to 5. We also give an analytic fit with numerical coefficients for approximating $\\tau(E_{\\gamma}, z)$. As an example of the application of our results, we calculate the absorbed spectrum of the blazar PKS 2155-304 at z = 0.117 and compare it with the spectrum observed by the H.E.S.S. air Cherenkov gamma-ray telescope array.

F. W. Stecker; M. A. Malkan; S. T. Scully

2006-05-25T23:59:59.000Z

150

TenTen: A New Array of Multi-TeV Imaging Cherenkov Telescopes  

E-Print Network [OSTI]

The exciting results from H.E.S.S. point to a new population of gamma-ray sources at energies E > 10 TeV, paving the way for future studies and new discoveries in the multi-TeV energy range. Connected with these energies is the search for sources of PeV cosmic-rays (CRs) and the study of multi-TeV gamma-ray production in a growing number of astrophysical environments. TenTen is a proposed stereoscopic array (with a suggested site in Australia) of modest-sized (10 to 30m^2) Cherenkov imaging telescopes with a wide field of view (8 to 10deg diameter) optimised for the E~10 to 100 TeV range. TenTen will achieve an effective area of ~10 km^2 at energies above 10 TeV. We outline here the motivation for TenTen and summarise key performance parameters.

Rowell, G; Clay, R; Dawson, B; Denman, J; Protheroe, R; Smith, A G K; Thornton, G; Wild, N

2007-01-01T23:59:59.000Z

151

TenTen: A New Array of Multi-TeV Imaging Cherenkov Telescopes  

E-Print Network [OSTI]

The exciting results from H.E.S.S. point to a new population of gamma-ray sources at energies E > 10 TeV, paving the way for future studies and new discoveries in the multi-TeV energy range. Connected with these energies is the search for sources of PeV cosmic-rays (CRs) and the study of multi-TeV gamma-ray production in a growing number of astrophysical environments. TenTen is a proposed stereoscopic array (with a suggested site in Australia) of modest-sized (10 to 30m^2) Cherenkov imaging telescopes with a wide field of view (8 to 10deg diameter) optimised for the E~10 to 100 TeV range. TenTen will achieve an effective area of ~10 km^2 at energies above 10 TeV. We outline here the motivation for TenTen and summarise key performance parameters.

G. Rowell; V. Stamatescu; R. Clay; B. Dawson; J. Denman; R. Protheroe; A. G. K. Smith; G. Thornton; N. Wild

2007-10-10T23:59:59.000Z

152

The exceptionally powerful TeV gamma-ray emitters in the Large Magellanic Cloud  

E-Print Network [OSTI]

The Large Magellanic Cloud, a satellite galaxy of the Milky Way, has been observed with the High Energy Stereoscopic System (H.E.S.S.) above an energy of 100 billion electron volts for a deep exposure of 210 hours. Three sources of different types were detected: the pulsar wind nebula of the most energetic pulsar known N 157B, the radio-loud supernova remnant N 132D and the largest non-thermal X-ray shell - the superbubble 30 Dor C. The unique object SN 1987A is, surprisingly, not detected, which constrains the theoretical framework of particle acceleration in very young supernova remnants. These detections reveal the most energetic tip of a gamma-ray source population in an external galaxy, and provide via 30 Dor C the unambiguous detection of gamma-ray emission from a superbubble.

:,; Aharonian, F; Benkhali, F Ait; Akhperjanian, A G; Angüner, E O; Backes, M; Balenderan, S; Balzer, A; Barnacka, A; Becherini, Y; Becker-Tjus, J; Berge, D; Bernhard, S; Bernlöhr, K; Birsin, E; Biteau, J; Böttcher, M; Boisson, C; Bolmont, J; Bordas, P; Bregeon, J; Brun, F; Brun, P; Bryan, M; Bulik, T; Carrigan, S; Casanova, S; Chadwick, P M; Chakraborty, N; Chalme-Calvet, R; Chaves, R C G; Chrétien, M; Colafrancesco, S; Cologna, G; Conrad, J; Couturier, C; Cui, Y; Dalton, M; Davids, I D; Degrange, B; Deil, C; de Wilt, P; Djannati-Ataï, A; Domainko, W; Donath, A; Drury, L O'C; Dubus, G; Dutson, K; Dyks, J; Dyrda, M; Edwards, T; Egberts, K; Eger, P; Espigat, P; Farnier, C; Fegan, S; Feinstein, F; Fernandes, M V; Fernandez, D; Fiasson, A; Fontaine, G; Förster, A; ling, M Füß; Gabici, S; Gajdus, M; Gallant, Y A; Garrigoux, T; Giavitto, G; Giebels, B; Glicenstein, J F; Gottschall, D; Grondin, M -H; Grudzi?ska, M; Hadasch, D; Häffner, S; Hahn, J; Harris, J; Heinzelmann, G; Henri, G; Hermann, G; Hervet, O; Hillert, A; Hinton, J A; Hofmann, W; Hofverberg, P; Holler, M; Horns, D; Ivascenko, A; Jacholkowska, A; Jahn, C; Jamrozy, M; Janiak, M; Jankowsky, F; Jung, I; Kastendieck, M A; Katarzy?ski, K; Katz, U; Kaufmann, S; Khélifi, B; Kieffer, M; Klepser, S; Klochkov, D; Klu?niak, W; Kolitzus, D; Komin, Nu; Kosack, K; Krakau, S; Krayzel, F; Krüger, P P; Laffon, H; Lamanna, G; Lefaucheur, J; Lefranc, V; Lemière, A; Lemoine-Goumard, M; Lenain, J -P; Lohse, T; Lopatin, A; Lu, C -C; Marandon, V; Marcowith, A; Marx, R; Maurin, G; Maxted, N; Mayer, M; McComb, T J L; Méhault, J; Meintjes, P J; Menzler, U; Meyer, M; Mitchell, A M W; Moderski, R; Mohamed, M; Morå, K; Moulin, E; Murach, T; de Naurois, M; Niemiec, J; Nolan, S J; Oakes, L; Odaka, H; Ohm, S; Opitz, B; Ostrowski, M; Oya, I; Panter, M; Parsons, R D; Arribas, M Paz; Pekeur, N W; Pelletier, G; Perez, J; Petrucci, P -O; Peyaud, B; Pita, S; Poon, H; Pühlhofer, G; Punch, M; Quirrenbach, A; Raab, S; Reichardt, I; Reimer, A; Reimer, O; Renaud, M; Reyes, R de los; Rieger, F; Rob, L; Romoli, C; Rosier-Lees, S; Rowell, G; Rudak, B; Sahakian, C B Rulten V; Salek, D; Sanchez, D A; Santangelo, A; Schlickeiser, R; Schüssler, F; Schulz, A; Schwanke, U; Schwarzburg, S; Schwemmer, S; Sol, H; Spanier, F; Spengler, G; Spies, F; Stawarz, ?; Steenkamp, R; Stegmann, C; Stinzing, F; Stycz, K; Sushch, I; Tavernet, J -P; Tavernier, T; Taylor, A M; Terrier, R; Tluczykont, M; Trichard, C; Valerius, K; van Eldik, C; van Soelen, B; Vasileiadis, G; Veh, J; Venter, C; Viana, A; Vincent, P; Vink, J; Völk, H J; Volpe, F; Vorster, M; Vuillaume, T; Wagner, S J; Wagner, P; Wagner, R M; Ward, M; Weidinger, M; Weitzel, Q; White, R; Wierzcholska, A; Willmann, P; Wörnlein, A; Wouters, D; Yang, R; Zabalza, V; Zaborov, D; Zacharias, M; Zdziarski, A A; Zech, A; Zechlin, H -S

2015-01-01T23:59:59.000Z

153

The AGASA/SUGAR Anisotropies and TeV Gamma Rays from the Galactic Center: A Possible Signature of Extremely High-energy Neutrons  

E-Print Network [OSTI]

Recent analysis of data sets from two extensive air shower cosmic ray detectors shows tantalizing evidence of an anisotropic overabundance of cosmic rays towards the Galactic Center (GC) that ``turns on'' around $10^{18}$ eV. We demonstrate that the anisotropy could be due to neutrons created at the Galactic Center through charge-exchange in proton-proton collisions, where the incident, high energy protons obey an $\\sim E^{-2}$ power law associated with acceleration at a strong shock. We show that the normalization supplied by the gamma-ray signal from EGRET GC source 3EG J1746-2851 -- ascribed to pp induced neutral pion decay at GeV energies -- together with a very reasonable spectral index of 2.2, predicts a neutron flux at $\\sim 10^{18}$ eV fully consistent with the extremely high energy cosmic ray data. Likewise, the normalization supplied by the very recent GC data from the HESS air-Cerenkov telescope at \\~TeV energies is almost equally-well compatible with the $\\sim 10^{18}$ eV cosmic ray data. Interestingly, however, the EGRET and HESS data appear to be themselves incompatible. We consider the implications of this discrepancy. We discuss why the Galactic Center environment can allow diffusive shock acceleration at strong shocks up to energies approaching the ankle in the cosmic ray spectrum. Finally, we argue that the shock acceleration may be occuring in the shell of Sagittarius A East, an unusual supernova remnant located very close to the Galactic Center. If this connection between the anisotropy and Sagittarius A East could be firmly established it would be the first direct evidence for a particular Galactic source of cosmic rays up to energies near the ankle.

Roland M. Crocker; Marco Fatuzzo; Randy Jokipii; Fulvio Melia; Raymond R. Volkas

2004-08-10T23:59:59.000Z

154

X-RAY OBSERVATIONS OF THE NEW UNUSUAL MAGNETAR SWIFT J1834.9-0846  

SciTech Connect (OSTI)

We present X-ray observations of the new transient magnetar Swift J1834.9-0846, discovered with the Swift Burst Alert Telescope on 2011 August 7. The data were obtained with Swift, Rossi X-ray Timing Explorer (RXTE), CXO, and XMM-Newton both before and after the outburst. Timing analysis reveals single peak pulsations with a period of 2.4823 s and an unusually high pulsed fraction, 85% {+-} 10%. Using the RXTE and CXO data, we estimated the period derivative, P-dot =8 Multiplication-Sign 10{sup -12} s s{sup -1}, and confirmed the high magnetic field of the source, B = 1.4 Multiplication-Sign 10{sup 14} G. The decay of the persistent X-ray flux, spanning 48 days, is consistent with a power law, F{proportional_to}t{sup -0.5}. In the CXO/Advanced CCD Imaging Spectrometer image, we find that the highly absorbed point source is surrounded by extended emission, which most likely is a dust scattering halo. Swift J1834.9-0846 is located near the center of the radio supernova remnant W41 and TeV source HESS J1834-087. An association with W41 would imply a source distance of about 4 kpc; however, any relation to the HESS source remains unclear, given the presence of several other candidate counterparts for the latter source in the field. Our search for an IR counterpart of Swift J1834.9-0846 revealed no source down to K{sub s} {approx} 19.5 within the 0.''6 CXO error circle.

Kargaltsev, Oleg [Department of Astronomy, Bryant Space Science Center, University of Florida, Gainesville, FL 32611 (United States); Kouveliotou, Chryssa; Younes, George [Science and Technology Office, ZP12, NASA/Marshall Space Flight Center, Huntsville, AL 35812 (United States); Pavlov, George G. [Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802 (United States); Goegues, Ersin; Lin, Lin; Kaneko, Yuki [Faculty of Engineering and Natural Sciences, Sabanc Latin-Small-Letter-Dotless-I University, Orhanl Latin-Small-Letter-Dotless-I -Tuzla, Istanbul 34956 (Turkey); Wachter, Stefanie; Griffith, Roger L., E-mail: oyk100@astro.ufl.edu [Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125 (United States)

2012-03-20T23:59:59.000Z

155

ARRA-Multi-Level Energy Storage and Controls for Large-Scale Wind Energy Integration  

SciTech Connect (OSTI)

The Project Objective is to design innovative energy storage architecture and associated controls for high wind penetration to increase reliability and market acceptance of wind power. The project goals are to facilitate wind energy integration at different levels by design and control of suitable energy storage systems. The three levels of wind power system are: Balancing Control Center level, Wind Power Plant level, and Wind Power Generator level. Our scopes are to smooth the wind power fluctuation and also ensure adequate battery life. In the new hybrid energy storage system (HESS) design for wind power generation application, the boundary levels of the state of charge of the battery and that of the supercapacitor are used in the control strategy. In the controller, some logic gates are also used to control the operating time durations of the battery. The sizing method is based on the average fluctuation of wind profiles of a specific wind station. The calculated battery size is dependent on the size of the supercapacitor, state of charge of the supercapacitor and battery wear. To accommodate the wind power fluctuation, a hybrid energy storage system (HESS) consisting of battery energy system (BESS) and super-capacitor is adopted in this project. A probability-based power capacity specification approach for the BESS and super-capacitors is proposed. Through this method the capacities of BESS and super-capacitor are properly designed to combine the characteristics of high energy density of BESS and the characteristics of high power density of super-capacitor. It turns out that the super-capacitor within HESS deals with the high power fluctuations, which contributes to the extension of BESS lifetime, and the super-capacitor can handle the peaks in wind power fluctuations without the severe penalty of round trip losses associated with a BESS. The proposed approach has been verified based on the real wind data from an existing wind power plant in Iowa. An intelligent controller that increases battery life within hybrid energy storage systems for wind application was developed. Comprehensive studies have been conducted and simulation results are analyzed. A permanent magnet synchronous generator, coupled with a variable speed wind turbine, is connected to a power grid (14-bus system). A rectifier, a DC-DC converter and an inverter are used to provide a complete model of the wind system. An Energy Storage System (ESS) is connected to a DC-link through a DC-DC converter. An intelligent controller is applied to the DC-DC converter to help the Voltage Source Inverter (VSI) to regulate output power and also to control the operation of the battery and supercapacitor. This ensures a longer life time for the batteries. The detailed model is simulated in PSCAD/EMTP. Additionally, economic analysis has been done for different methods that can reduce the wind power output fluctuation. These methods are, wind power curtailment, dumping loads, battery energy storage system and hybrid energy storage system. From the results, application of single advanced HESS can save more money for wind turbines owners. Generally the income would be the same for most of methods because the wind does not change and maximum power point tracking can be applied to most systems. On the other hand, the cost is the key point. For short term and small wind turbine, the BESS is the cheapest and applicable method while for large scale wind turbines and wind farms the application of advanced HESS would be the best method to reduce the power fluctuation. The key outcomes of this project include a new intelligent controller that can reduce energy exchanged between the battery and DC-link, reduce charging/discharging cycles, reduce depth of discharge and increase time interval between charge/discharge, and lower battery temperature. This improves the overall lifetime of battery energy storages. Additionally, a new design method based on probability help optimize the power capacity specification for BESS and super-capacitors. Recommendations include experimental imp

David Wenzhong Gao

2012-09-30T23:59:59.000Z

156

A Persistent High-Energy Flux from the Heart of the Milky Way : Integral's view of the Galactic Center  

E-Print Network [OSTI]

The Ibis/Isgri imager on Integral detected for the first time a hard X-ray source, IGR J17456-2901, located within 1' of Sgr A* over the energy range 20-100 keV. Here we present the results of a detailed analysis of ~7 Ms of Integral observations of the GC. With an effective exposure of 4.7 Ms we have obtained more stringent positional constraints on this HE source and constructed its spectrum in the range 20-400 keV. Furthermore, by combining the Isgri spectrum with the total X-ray spectrum corresponding to the same physical region around SgrA* from XMM data, and collected during part of the Integral observations, we constructed and present the first accurate wide band HE spectrum for the central arcmins of the Galaxy. Our complete analysis of the emission properties of IGR shows that it is faint but persistent with no variability above 3 sigma contrary to what was alluded to in our first paper. This result, in conjunction with the spectral characteristics of the X-ray emission from this region, suggests that the source is most likely not point-like but, rather, that it is a compact, yet diffuse, non-thermal emission region. The centroid of IGR is estimated to be R.A.=17h45m42.5, decl.=-28deg59'28'', offset by 1' from the radio position of Sgr A* and with a positional uncertainty of 1'. Its 20-400 keV luminosity at 8 kpc is L=5.4x10^35 erg/sec. Very recently, Hess detected of a source of ~TeV g-rays also located within 1' of Sgr A*. We present arguments in favor of an interpretation according to which the photons detected by Integral and Hess arise from the same compact region of diffuse emission near the central BH and that the supernova remnant Sgr A East could play an important role as a contributor of very HE g-rays to the overall spectrum from this region.

Guillaume Belanger; Andrea Goldwurm; Matthieu Renaud; Regis Terrier; Fulvio Melia; Niels Lund; Jacques Paul; Gerry Skinner; Farah Yusef-Zadeh

2005-08-04T23:59:59.000Z

157

Cosmic-ray induced gamma-ray emission from the starburst galaxy NGC 253  

SciTech Connect (OSTI)

Cosmic rays in galaxies interact with the interstellar medium and give us a direct view of nuclear and particle interactions in the cosmos. For example, cosmic-ray proton interactions with interstellar hydrogen produce gamma rays via PcrPism??{sup 0}???. For a 'normal' star-forming galaxy like the Milky Way, most cosmic rays escape the Galaxy before such collisions, but in starburst galaxies with dense gas and huge star formation rate, most cosmic rays do suffer these interactions [1,2]. We construct a 'thick-target' model for starburst galaxies, in which cosmic rays are accelerated by supernovae, and escape is neglected. This model gives an upper limit to the gamma-ray emission. Only two free parameters are involved in the model: cosmic-ray proton acceleration energy rate from supernova and the proton injection spectral index. The pionic gamma-radiation is calculated from 10 MeV to 10 TeV for the starburst galaxy NGC 253, and compared to Fermi and HESS data. Our model fits NGC 253 well, suggesting that cosmic rays in this starburst are in the thick target limit, and that this galaxy is a gamma-ray calorimeter.

Wang, Xilu; Fields, Brian D. [Department of Astronomy, MC-221, 1002 W. Green Street, University of Illinois at Urbana-Champaign, Urbana, IL 61801 (United States)

2014-05-09T23:59:59.000Z

158

The hard TeV spectrum of 1ES 0229+200: new clues from Swift  

E-Print Network [OSTI]

The BL Lac object 1ES 0229+200 (z=0.14) has been detected by HESS during observations taking place in 2005-2006. The TeV spectrum, when corrected for the absorption of gamma-ray photons through the interaction with the extragalactic background light, is extremely hard, even if the most conservative level for the background is considered. The case of 1ES 0229+200 is very similar to that of 1ES 1101-232, for which a possible explanation, in the framework of the standard one-zone synchrotron-self Compton model, is that the high-energy emission is synchrotron-self Compton radiation of electrons distributed as a power law with a large value of the minimum energy. In this scenario the hard TeV spectrum is accompanied by a very hard synchrotron continuum below the soft X-ray band. We will show that recent Swift observations of 1ES 0229+200 in the critical UV-X-ray band strongly support this model, showing the presence of the expected spectral break and hard continuum between the UV and the X-ray bands.

Tavecchio, F; Ghirlanda, G; Franceschini, A

2009-01-01T23:59:59.000Z

159

Advanced Microturbine Systems  

SciTech Connect (OSTI)

Dept. of Energy (DOE) Cooperative Agreement DE-FC02-00-CH11061 was originally awarded to Honeywell International, Inc. â?? Honeywell Power Systems Inc. (HPSI) division located in Albuquerque, NM in October 2000 to conduct a program titled Advanced Microturbine Systems (AMS). The DOE Advanced Microturbines Systems Program was originally proposed as a five-year program to design and develop a high efficiency, low emissions, durable microturbine system. The period of performance was to be October 2000 through September 2005. Program efforts were underway, when one year into the program Honeywell sold the intellectual property of Honeywell Power Systems Inc. and HPSI ceased business operations. Honeywell made an internal decision to restructure the existing program due to the HPSI shutdown and submitted a formal request to DOE on September 24, 2001 to transfer the Cooperative Agreement to Honeywell Engines, Systems and Services (HES&S) in Phoenix, AZ in order to continue to offer support for DOE's Advanced Microturbine Program. Work continued on the descoped program under Cooperative Agreement No. DE-FC26-00-CH11061 and has been completed.

None

2005-12-31T23:59:59.000Z

160

Investigating gamma-ray lines from dark matter with future observatories  

SciTech Connect (OSTI)

We study the prospects for studying line features in gamma-ray spectra with upcoming gamma-ray experiments, such as HESS-II, the Cherenkov Telescope Array (CTA), and the GAMMA-400 satellite. As an example we use the narrow feature at 130 GeV seen in public data from the Fermi-LAT satellite. We found that all three experiments should be able to confidently confirm or rule out the presence of this 130 GeV feature. If it is real, it should be confirmed with a confidence level higher than 5?. Assuming it to be a spectral signature of dark matter origin, GAMMA-400, thanks to a projected energy resolution of about 1.5 % at 100 GeV, should also be able to resolve both the ?? line and a corresponding Z? or H? feature, if the corresponding branching ratio is comparable to that into two photons. It will also allow to distinguish between a gamma-ray line and the similar feature resulting from internal bremsstrahlung photons.

Bergström, Lars; Conrad, Jan; Farnier, Christian [The Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm (Sweden); Bertone, Gianfranco [GRAPPA Institute, University of Amsterdam, Science Park 904, 1090 GL Amsterdam (Netherlands); Weniger, Christoph, E-mail: lbe@fysik.su.se, E-mail: gf.bertone@gmail.com, E-mail: conrad@fysik.su.se, E-mail: Christian.Farnier@fysik.su.se, E-mail: weniger@mpp.mpg.de [Max-Planck-Institut für Physik, Föhringer Ring 6, 80805 München (Germany)

2012-11-01T23:59:59.000Z

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161

Radio Synchrotron Emission from Secondary Leptons in the Vicinity of Sgr A*  

E-Print Network [OSTI]

A point-like source of ~TeV gamma-rays has recently been seen towards the Galactic center by HESS and other air Cerenkov telescopes. In recent work (Ballantyne et al. 2007), we demonstrated that these gamma-rays can be attributed to high-energy protons that (i) are accelerated close to the event horizon of the central black hole, Sgr A*, (ii) diffuse out to ~pc scales, and (iii) finally interact to produce gamma-rays. The same hadronic collision processes will necessarily lead to the creation of electrons and positrons. Here we calculate the synchrotron emissivity of these secondary leptons in the same magnetic field configuration through which the initiating protons have been propagated in our model. We compare this emission with the observed ~GHz radio spectrum of the inner few pc region which we have assembled from archival data and new measurements we have made with the Australia Telescope Compact Array. We find that our model predicts secondary synchrotron emission with a steep slope consistent with the observations but with an overall normalization that is too large by a factor of ~ 2. If we further constrain our theoretical gamma-ray curve to obey the implicit EGRET upper limit on emission from this region we predict radio emission that is consistent with observations, i.e., the hadronic model of gamma ray emission can, simultaneously and without fine-tuning, also explain essentially all the diffuse radio emission detected from the inner few pc of the Galaxy.

Roland M. Crocker; David Jones; David R. Ballantyne; Fulvio Melia

2007-08-07T23:59:59.000Z

162

Linking radio and gamma ray emission in Ap Librae  

E-Print Network [OSTI]

Ap Lib is one of the rare Low Synchrotron Peaked blazars detected so far at TeV energies. This type of source is not properly modelled by standard one-zone leptonic Synchrotron-self-Compton (SSC) emission scenarios. The aim of this paper is to study the relevance of additional components which should naturally occur in a SSC scenario for a better understanding of the emission mechanisms, especially at very high energies (VHE). Methods. We use simultaneous data from a multi-wavelength campaign of Planck, Swift-UVOT and Swift-XRT telescopes carried out in February 2010, as well as quasi-simultaneous data of WISE, Fermi and H.E.S.S. taken in 2010. The multi-lambda emission of Ap Lib is modelled by a blob-in-jet SSC scenario including the contribution of the base of the VLBI extended jet, the radiative blob-jet interaction, the accretion disk and its associated external photon field. We show that signatures of a strong parsec-scale jet and of an accretion disk emission are present in the SED. We can link the obse...

Hervet, O; Sol, H

2015-01-01T23:59:59.000Z

163

How precisely neutrino emission from supernova remnants can be constrained by gamma ray observations?  

E-Print Network [OSTI]

We propose a conceptually and computationally simple method to evaluate the neutrinos emitted by supernova remnants using the observed gamma-ray spectrum. The proposed method does not require any preliminary parametrization of the gamma ray flux; the gamma ray data can be used as an input. In this way, we are able to propagate easily the observational errors and to understand how well the neutrino flux and the signal in neutrino telescopes can be constrained by gamma-ray data. We discuss the various possible sources of theoretical and systematical uncertainties (e.g., neutrino oscillation parameters, hadronic modeling, etc.), obtaining an estimate of the accuracy of our calculation. Furthermore, we apply our approach to the supernova remnant RX J1713.7-3946, showing that neutrino emission is very-well constrained by the H.E.S.S. gamma-ray data: indeed, the accuracy of our prediction is limited by theoretical uncertainties. Neutrinos from RX J1713.7-3946 can be detected with an exposure of the order km^2 year, provided that the detection threshold in future neutrino telescopes will be equal to about 1 TeV.

F. L. Villante; F. Vissani

2008-07-25T23:59:59.000Z

164

Method to extract the primary cosmic ray spectrum from very high energy gamma-ray data and its application to SNR RX J1713.7-3946  

E-Print Network [OSTI]

Supernova remnants are likely to be the accelerators of the galactic cosmic rays. Assuming the correctness of this hypothesis, we develop a method to extract the parent cosmic ray spectrum from the VHE gamma ray flux emitted by supernova remnants (and other gamma transparent sources). Namely, we calculate semi-analytically the (inverse) operator which relates an arbitrary gamma ray flux to the parent cosmic ray spectrum, without relying on any theoretical assumption about the shape of the cosmic ray and/or photon spectrum. We illustrate the use of this technique by applying it to the young SNR RX J1713.7-3946 which has been observed by H.E.S.S. experiment during the last three years. Specific implementations of the method permit to use as an input either the parameterized VHE gamma ray flux or directly the raw data. The possibility to detect features in the cosmic rays spectrum and the error in the determination of the parent cosmic ray spectrum are also discussed.

F. L. Villante; F. Vissani

2008-01-04T23:59:59.000Z

165

On the formation of TeV radiation in LS 5039  

E-Print Network [OSTI]

The recent detections of TeV gamma-rays from compact binary systems show that relativistic outflows (jets or winds) are sites of effective acceleration of particles up to multi-TeV energies. In this paper, we discuss the conditions of acceleration and radiation of ultra-relativistic electrons in LS 5039, the gamma-ray emitting binary system for which the highest quality TeV data are available. Assuming that the gamma-ray emitter is a jet-like structure, we performed detailed numerical calculations of the energy spectrum and lightcurves accounting for the acceleration efficiency, the location of the accelerator, the speed of the emitting flow, the inclination angle of the system, as well as specific features related to anisotropic inverse Compton scattering and pair production. We conclude that the accelerator should not be deep inside the binary system unless we assume a very efficient acceleration rate. We show that within the IC scenario both the gamma-ray spectrum and flux are strongly orbital phase dependent. Formally, our model can reproduce, for specific sets of parameter values, the energy spectrum of gamma-rays reported by HESS for wide orbital phase intervals. However, the physical properties of the source can be constrained only by observations capable of providing detailed energy spectra for narrow orbital phase intervals ($\\Delta\\phi\\ll 0.1$).

Dmitry Khangulyan; Felix Aharonian; Valenti Bosch-Ramon

2007-10-10T23:59:59.000Z

166

Gamma-ray Astronomy: Implications for Fundamental Physics  

E-Print Network [OSTI]

Gamma-ray Astronomy studies cosmic accelerators through their electromagnetic radiation in the energy range between ~100 MeV and ~100 TeV. The present most sensitive observations in this energy band are performed, from space, by the Large Area Telescope onboard the Fermi satellite and, from Earth, by the Imaging Air Cherenkov Telescopes MAGIC, H.E.S.S. and VERITAS. These instruments have revolutionized the field of Gamma-ray Astronomy, discovering different populations of gamma-ray emitters and studying in detail the non-thermal astrophysical processes producing this high-energy radiation. The scientific objectives of these observatories include also questions of fundamental physics. With gamma-ray instruments we study the origin of Galactic cosmic rays, testing the hypothesis or whether they are mainly produced in supernova explosions. Also, we obtain the most sensitive measurement of the cosmic electron-positron spectrum between 20 GeV and 5 TeV. By observing the gamma-ray emission from sources at cosmological distances, we learn about the intensity and evolution of the extragalactic background light, and perform tests of Lorentz Invariance. Moreover, we can search for dark matter by looking for gamma-ray signals produced by its annihilation or decay in over-density sites. In this paper, we review the most recent results produced with the current generation of gamma-ray instruments in these fields of research.

Javier Rico

2011-11-28T23:59:59.000Z

167

The GeV-TeV Connection in Galactic gamma-ray Sources  

SciTech Connect (OSTI)

Recent observations by atmospheric Cherenkov telescopes such as H.E.S.S. and MAGIC have revealed a large number of new sources of very-high-energy (VHE) gamma-rays above 100 GeV, mostly concentrated along the Galactic plane. At lower energies (100 MeV - 10 GeV) the satellite-based instrument EGRET revealed a population of sources clustering along the Galactic Plane. Given their adjacent energy bands a systematic correlation study between the two source classes seems appropriate. While only a few of the sources connect, both in terms of positional coincidence and spectral consistency, most of the detections occur only in one or the other energy domain. In these cases, for the first time consistent upper limits in the other energy band have been derived. Here, the populations of Galactic sources in both energy domains are characterized on observational as well as on theoretical grounds, followed by an interpretation on their similarities and differences. The observational data at this stage suggest rather different major source populations at GeV and TeV energies. With regards to preparations for the upcoming GLAST mission that will cover the energy range bridging GeV and TeV instruments this paper investigates the connection between the population of sources in these bands and concludes with predictions for commonly observable sources for GLAST-LAT detections.

Funk, S.; /KIPAC, Menlo Park; Reimer, O.; /Stanford U., HEPL /KIPAC, Menlo Park; Torres, Diego F.; /ICREA, Barcelona; Hinton, J.A.; /Leeds U.

2007-09-28T23:59:59.000Z

168

Development of a mid-sized Schwarzschild-Couder Telescope for the Cherenkov Telescope Array  

SciTech Connect (OSTI)

The Cherenkov Telescope Array (CTA) is a ground-based observatory for very high-energy (10 GeV to 100 TeV) gamma rays, planned for operation starting in 2018. It will be an array of dozens of optical telescopes, known as Atmospheric Cherenkov Telescopes (ACTs), of 8 m to 24 m diameter, deployed over an area of more than 1 square km, to detect flashes of Cherenkov light from showers initiated in the Earth's atmosphere by gamma rays. CTA will have improved angular resolution, a wider energy range, larger fields of view and an order of magnitude improvement in sensitivity over current ACT arrays such as H.E.S.S., MAGIC and VERITAS. Several institutions have proposed a research and development program to eventually contribute 36 medium-sized telescopes (9 m to 12 m diameter) to CTA to enhance and optimize its science performance. The program aims to construct a prototype of an innovative, Schwarzschild-Couder telescope (SCT) design that will allow much smaller and less expensive cameras and much larger fields of view than conventional Davies-Cotton designs, and will also include design and testing of camera electronics for the necessary advances in performance, reliability and cost. We report on the progress of the mid-sized SCT development program.

Cameron, Robert A.

2012-06-28T23:59:59.000Z

169

Search for Lorentz Invariance breaking with a likelihood fit of the PKS 2155-304 flare data taken on MJD 53944  

E-Print Network [OSTI]

Several models of Quantum Gravity predict Lorentz Symmetry breaking at energy scales approaching the Planck scale (10^{19} GeV). With present photon data from the observations of distant astrophysical sources, it is possible to constrain the Lorentz Symmetry breaking linear term in the standard photon dispersion relations. Gamma-ray Bursts (GRB) and flaring Active Galactic Nuclei (AGN) are complementary to each other for this purpose, since they are observed at different distances in different energy ranges and with different levels of variability. Following a previous publication of the High Energy Stereoscopic System (H.E.S.S.) collaboration, a more sensitive event-by-event method consisting of a likelihood fit is applied to PKS 2155-304 flare data of MJD 53944 (July 28, 2006) as used in the previous publication. The previous limit on the linear term is improved by a factor of ~3 up to M^{l}_{QG} > 2.1x10^{18} GeV and is currently the best result obtained with blazars. The sensitivity to the quadratic term is lower and provides a limit of M^{q}_{QG} > 6.4x10^10 GeV, which is the best value obtained so far with an AGN and similar to the best limits obtained with GRB.

HESS Collaboration; A. Abramowski; F. Acero; F. Aharonian; A. G. Akhperjanian; G. Anton; A. Barnacka; U. Barres de Almeida; A. R. Bazer-Bachi; Y. Becherini; J. Becker; B. Behera; K. Bernlöhr; A. Bochow; C. Boisson; J. Bolmont; P. Bordas; V. Borrel; J. Brucker; F. Brun; P. Brun; T. Bulik; I. Büsching; R. Bühler; S. Carrigan; S. Casanova; M. Cerruti; P. M. Chadwick; A. Charbonnier; R. C. G. Chaves; A. Cheesebrough; L. -M. Chounet; A. C. Clapson; G. Coignet; J. Conrad; M. Dalton; M. K. Daniel; I. D. Davids; B. Degrange; C. Deil; H. J. Dickinson; A. Djannati-Ataï; W. Domainko; L. O'C. Drury; F. Dubois; G. Dubus; J. Dyks; M. Dyrda; K. Egberts; P. Eger; P. Espigat; L. Fallon; C. Farnier; S. Fegan; F. Feinstein; M. V. Fernandes; A. Fiasson; A. Frster; G. Fontaine; M. Füßling; Y. A. Gallant; H. Gast; L. Gérard; D. Gerbig; B. Giebels; J. F. Glicenstein; B. Glück; P. Goret; D. Göring; J. D. Hague; D. Hampf; M. Hauser; S. Heinz; G. Heinzelmann; G. Henri; G. Hermann; J. A. Hinton; A. Hoffmann; W. Hofmann; P. Hofverberg; D. Horns; A. Jacholkowska; O. C. de Jager; C. Jahn; M. Jamrozy; I. Jung; M. A. Kastendieck; K. Katarzy?ski; U. Katz; S. Kaufmann; D. Keogh; M. Kerschhaggl; D. Khangulyan; B. Khélifi; D. Klochkov; W. Klu?niak; T. Kneiske; Nu. Komin; K. Kosack; R. Kossakowski; H. Laffon; G. Lamanna; D. Lennarz; T. Lohse; A. Lopatin; C. -C. Lu; V. Marandon; A. Marcowith; J. Masbou; D. Maurin; N. Maxted; T. J. L. McComb; M. C. Medina; J. Méhault; R. Moderski; E. Moulin; C. L. Naumann; M. Naumann-Godo; M. de Naurois; D. Nedbal; D. Nekrassov; N. Nguyen; B. Nicholas; J. Niemiec; S. J. Nolan; S. Ohm; J-F. Olive; E. de Oña Wilhelmi; B. Opitz; M. Ostrowski; M. Panter; M. Paz Arribas; G. Pedaletti1; G. Pelletier; P. -O. Petrucci; S. Pita; G. Pühlhofer; M. Punch; A. Quirrenbach; M. Raue; S. M. Rayner; A. Reimer; O. Reimer; M. Renaud; R. de los Reyes; F. Rieger; J. Ripken; L. Rob; S. Rosier-Lees; G. Rowell; B. Rudak; C. B. Rulten; J. Ruppel; F. Ryde; V. Sahakian; A. Santangelo; R. Schlickeiser; F. M. Schöck; A. Schönwald; U. Schwanke; S. Schwarzburg; S. Schwemmer; A. Shalchi; M. Sikora; J. L. Skilton; H. Sol; G. Spengler; ?. Stawarz; R. Steenkamp; C. Stegmann; F. Stinzing; I. Sushch; A. Szostek; J. -P. Tavernet; R. Terrier; O. Tibolla; M. Tluczykont; K. Valerius; C. van Eldik; G. Vasileiadis; C. Venter; J. P. Vialle; A. Viana; P. Vincent; M. Vivier; H. J. Völk; F. Volpe; S. Vorobiov; M. Vorster; S. J. Wagner; M. Ward; A. Wierzcholska; A. Zajczyk; A. A. Zdziarski; A. Zech; H. -S. Zechlin

2011-02-02T23:59:59.000Z

170

VERITAS Observations of the Galactic Center Ridge  

E-Print Network [OSTI]

Due to its extraordinarily high concentration of known relativistic particle accelerators such as pulsar wind nebula, supernova remnants, dense molecular cloud regions, and the supermassive black hole (Sgr A*); the center of the Milky Way galaxy has long been an ideal target for high energy (HE, 0.1-100 GeV) and very high energy ( VHE, 50 GeV-50 TeV) gamma-ray emission. Indeed, detections of Sgr A* and other nearby regions of gamma-ray emission have been reported by EGRET and Fermi-LAT in the HE band, as well as CANGAROO, Whipple, HESS, VERITAS, and MAGIC in the VHE band. Here we report on the results of extended observations of the region with VERITAS between 2010-2014. Due to the visibility of the source for VERITAS in the Northern Hemisphere, these observations provide the most sensitive probe of gamma-ray emission above 2 TeV in one of the most complicated and interesting regions of our home galaxy.

,

2015-01-01T23:59:59.000Z

171

A search for optical counterparts of the complex Vela X system  

E-Print Network [OSTI]

The pulsar wind nebula (PWN) associated with the Vela pulsar is a bright source in the radio, X-ray and gamma-ray bands, but not in the optical. This source is very near, lying at a distance of 290 pc, as inferred from the radio and optical parallax measurements of the pulsar. Knowledge of the brightness and structure of the Vela PWN in optical is important in order to constrain the underlying particle spectrum (and possibly the B-field properties and particle losses) associated with this extended source. We use results from the Digital Sky Survey, as well as results obtained using the SAAO 1.0 m telescope equipped with an imaging CCD (STE4) and BV filters, in an attempt to measure optical radiation from Vela X. To enlarge our field of view, we constructed a mosaic consisting of 3 x 3 frames around the pulsar position. We present spectral measurements from the High Energy Stereoscopic System (H.E.S.S.), Fermi Large Area Telescope (LAT), ASCA, Hubble Space Telescope (HST), Very Large Telescope (VLT), New Techn...

Marubini, T E; Venter, C; de Jager, O C

2015-01-01T23:59:59.000Z

172

Searching for Smoking Gun Signatures of Decaying Dark Matter  

E-Print Network [OSTI]

Clear methods to differentiate between decaying and annihilating dark matter (DM) scenarios are still by and large unavailable. In this note, we study the potential astrophysical signatures of a new class of hidden sector decaying DM models, which can address the recent cosmic ray measurements. Such models may produce primary photons and/or neutrinos at large rates, correlated with the leptonic production. The photon and neutrino spectra will then contain sharp features at the TeV scale. We demonstrate the discovery potential for upcoming and future measurements by FERMI, HESS, AGIS and IceCube/DeepCore. We show that these models may be discovered in the near future. Specifically, measurements of diffuse gamma rays by FERMI can detect the start of a hard photon feature. We argue that these hard spectra can be produced by decaying dark matter and be consistent with current constraints, but are difficult to reconcile with models of annihilating DM. Consequently the measurement of a hard spectral feature, in correlation with the current cosmic ray measurements, will strongly favor decaying DM models. Finally we comment on the preliminary results from the Inner Galaxy presented by the FERMI collaboration.

Joshua T. Ruderman; Tomer Volansky

2009-08-11T23:59:59.000Z

173

Towards SiPM camera for current and future generations of Cherenkov telescopes  

E-Print Network [OSTI]

So far the current ground-based Imaging Atmospheric Cherenkov Telescopes (IACTs) have energy thresholds in the best case in the range of ~30 to 50 GeV (H.E.S.S. II and MAGIC telescopes). Lowest energy gamma-ray showers produce low light intensity images and cannot be efficiently separated from dominating images from hadronic background. A cost effective way of improving the telescope performance at lower energies is to use novel photosensors with superior photon detection efficiency (PDE). Currently the best commercially available superbialkali photomultipliers (PMTs) have a PDE of about 30-33%, whereas the silicon photomultipliers (SiPMs, also known as MPPC, GAPD) from some manufacturers show a photon detection efficiency of about 40-45%. Using these devices can lower the energy threshold of the instrument and may improve the background rejection due to intrinsic properties of SiPMs such as a superb single photoelectron resolution. Compared to PMTs, SiPMs are more compact, fast in response, operate at low vo...

Mazin, Daniel; Sitarek, Julian; Cortina, Juan; Fink, David; Hose, Jürgen; Illa, Jose Maria; Lorenz, Eckart; Martínez, Manel; Menzel, Uta; Mirzoyan, Razmik; Teshima, Masahiro

2014-01-01T23:59:59.000Z

174

Galactic bursts signature in Antarctica 10Be  

E-Print Network [OSTI]

I detected a very strong (25 %var) period of 3592+-57 years at 99% confidence level in the 10Be deposition rates from Vostok, Antarctica ice core raw (gapped, unaltered) data. The period was verified at 99% confidence level against the 10Be concentration raw data at both Vostok, as 3700+-57 years at very strong 38 %var, and Taylor Dome, Antarctica, as 3800+-61 years at very strong 23 %var. The noisy Mg concentration data from Taylor Dome also show an extremely strong (44 %var) period of 3965+-16 years. The Vostok data also show the Hallstadzeit Solar cycle, as 2296+-57 years at 12 %var, perhaps its best estimate yet. I use for all analyses the 99% confidence strict Gauss-Vanicek spectral analysis (GVSA) that estimates periods in incomplete records. Based on recent 500-parsec Galactic Center (GC) GeV/TeV Gamma ray surveys by the H.E.S.S. and INTEGRAL telescopes, the GC extremely active central region makes the best candidate host for bursts leaving the discovered signature. A previously reported 3600 years per...

Omerbashich, M

2006-01-01T23:59:59.000Z

175

EVIDENCE FOR A SECOND COMPONENT IN THE HIGH-ENERGY CORE EMISSION FROM CENTAURUS A?  

SciTech Connect (OSTI)

We report on an analysis of Fermi Large Area Telescope data from four years of observations of the nearby radio galaxy Centaurus A (Cen A). The increased photon statistics results in a detection of high-energy (>100 MeV) gamma-rays up to 50 GeV from the core of Cen A, with a detection significance of about 44{sigma}. The average gamma-ray spectrum of the core reveals evidence for a possible deviation from a simple power law. A likelihood analysis with a broken power-law model shows that the photon index becomes harder above E{sub b} {approx_equal} 4 GeV, changing from {Gamma}{sub 1} = 2.74 {+-} 0.03 below to {Gamma}{sub 2} = 2.09 {+-} 0.20 above. This hardening could be caused by the contribution of an additional high-energy component beyond the common synchrotron self-Compton jet emission. No clear evidence for variability in the high-energy domain is seen. We compare our results with the spectrum reported by H.E.S.S. in the TeV energy range and discuss possible origins of the hardening observed.

Sahakyan, N. [ICRANet, Piazz della Repubblica 10, I-65122 Pescara (Italy); Yang, R. [Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, CAS, Nanjing 210008 (China); Aharonian, F. A. [Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2 (Ireland); Rieger, F. M. [Max-Planck-Institut fuer Kernphysik, P.O. Box 103980, D-69029 Heidelberg (Germany)

2013-06-10T23:59:59.000Z

176

MODELING PHOTODISINTEGRATION-INDUCED TeV PHOTON EMISSION FROM LOW-LUMINOSITY GAMMA-RAY BURSTS  

SciTech Connect (OSTI)

Ultra-high-energy cosmic-ray heavy nuclei have recently been considered as originating from nearby low-luminosity gamma-ray bursts that are associated with Type Ibc supernovae. Unlike the power-law decay in long duration gamma-ray bursts, the light curve of these bursts exhibits complex UV/optical behavior: shock breakout dominated thermal radiation peaks at about 1 day, and, after that, nearly constant emission sustained by radioactive materials for tens of days. We show that the highly boosted heavy nuclei at PeV energy interacting with the UV/optical photon field will produce considerable TeV photons via the photodisintegration/photo-de-excitation process. It was later predicted that a thermal-like {gamma}-ray spectrum peaks at about a few TeV, which may serve as evidence of nucleus acceleration. The future observations by the space telescope Fermi and by the ground atmospheric Cherenkov telescopes such as H.E.S.S., VERITAS, and MAGIC will shed light on this prediction.

Liu Xuewen [Physics Department, Sichuan University, Chengdu 610065 (China); Wu Xuefeng; Lu Tan, E-mail: astrolxw@gmail.com, E-mail: xfwu@pmo.ac.cn, E-mail: t.lu@pmo.ac.cn [Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008 (China)

2012-05-15T23:59:59.000Z

177

In Wino Veritas? Indirect Searches Shed Light on Neutralino Dark Matter  

E-Print Network [OSTI]

Indirect detection constraints on gamma rays (both continuum and lines) have set strong constraints on wino dark matter. By combining results from Fermi-LAT and HESS, we show that: light nonthermal wino dark matter is strongly excluded; thermal wino dark matter is allowed only if the Milky Way dark matter distribution has a significant (>~0.4 kpc) core; and for plausible NFW and Einasto distributions the entire range of wino masses from 100 GeV up to 3 TeV can be excluded. The case of light, nonthermal wino dark matter is particularly interesting in scenarios with decaying moduli that reheat the universe to a low temperature. Typically such models have been discussed for low reheating temperatures, not far above the BBN bound of a few MeV. We show that constraints on the allowed wino relic density push such models to higher reheating temperatures and hence heavier moduli. Even for a flattened halo model consisting of an NFW profile with constant-density core inside 1 kpc and a density near the sun of 0.3 GeV/...

Fan, JiJi

2013-01-01T23:59:59.000Z

178

Transmission integral analysis of Mössbauer spectra displaying hyperfine parameter distributions with arbitrary profile  

SciTech Connect (OSTI)

Accurate quantitative analysis of Mössbauer spectra displaying thickness effects requires the consideration of the so-called transmission integral when modeling the spectral shape. Whereas this is straightforward when the correct model for the decomposition of the absorber's nuclear resonance absorption cross-section into individual components is a priori known, in the absence of such knowledge and notably in the presence of hyperfine parameter distributions with an unknown profile, the so-called model-independent evaluation methods could be used to fit the spectra. However, the methods available for this purpose were developed for the analysis of spectra for which the thin absorber approximation is valid, and thus they do not take the sample thickness and related effects into account. Consequently, in order to use them for spectra displaying thickness effects, their usage needs to be generalized by combining them with transmission integral fitting. A new algorithm realizing such a generalized version of the Hesse-Rübartsch model-independent evaluation method was developed recently as an integral part of the MossWinn program. In the present work, the working principle of the newly developed algorithm is described in details along with examples illustrating the capabilities of the method for the case of {sup 57}Fe Mössbauer spectroscopy.

Klencsár, Zoltán, E-mail: z.klencsar@mosswinn.hu [Pitvar u. 11., Budapest 1141 (Hungary)

2014-10-27T23:59:59.000Z

179

PRE-MAIN-SEQUENCE STELLAR POPULATIONS ACROSS SHAPLEY CONSTELLATION III. I. PHOTOMETRIC ANALYSIS AND IDENTIFICATION ,  

SciTech Connect (OSTI)

We present our investigation of pre-main-sequence (PMS) stellar populations in the Large Magellanic Cloud (LMC) from imaging with Hubble Space Telescope Wide-Field Planetary Camera 2. Our targets of interest are four star-forming regions located at the periphery of the super-giant shell LMC 4 (Shapley Constellation III). The PMS stellar content of the regions is revealed through the differential Hess diagrams and the observed color-magnitude diagrams (CMDs). Further statistical analysis of stellar distributions along cross sections of the faint part of the CMDs allowed the quantitative assessment of the PMS stars census, and the isolation of faint PMS stars as the true low-mass stellar members of the regions. These distributions are found to be well represented by a double-Gaussian function, the first component of which represents the main-sequence field stars and the second the native PMS stars of each region. Based on this result, a cluster membership probability was assigned to each PMS star according to its CMD position. The higher extinction in the region LH 88 did not allow the unambiguous identification of its native stellar population. The CMD distributions of the PMS stars with the highest membership probability in the regions LH 60, LH 63, and LH 72 exhibit an extraordinary similarity among the regions, suggesting that these stars share common characteristics, as well as common recent star formation history. Considering that the regions are located at different areas of the edge of LMC 4, this finding suggests that star formation along the super-giant shell may have occurred almost simultaneously.

Gouliermis, Dimitrios A.; Gennaro, Mario; Henning, Thomas; Da Rio, Nicola; Brandner, Wolfgang [Max Planck Institute for Astronomy, Koenigstuhl 17, 69117 Heidelberg (Germany); Dolphin, Andrew E. [Raytheon Company, P.O. Box 11337, Tucson, AZ 85734 (United States); Robberto, Massimo; Panagia, Nino [Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218 (United States); Gruendl, Robert A.; Chu, You-Hua [Department of Astronomy, University of Illinois, 1002 West Green Street, Urbana, IL 61801 (United States); Rosa, Michael; Romaniello, Martino [ESO, Karl-Schwarzschild-Str. 2, 85748 Garching (Germany); De Marchi, Guido [ESA, Space Science Department, Keplerlaan 1, 2200 AG Noordwijk (Netherlands); Zinnecker, Hans [Institut fuer Raumfahrtsyteme, Universitaet Stuttgart, Pfaffenwaldring 31, 70569 Stuttgart (Germany)

2011-09-10T23:59:59.000Z

180

Neutrino Astronomy and Cosmic Rays Spectroscopy at Horizons  

E-Print Network [OSTI]

A new air-showering physics may rise in next years at horizon, offering at different angles and altitudes a fine tuned filtered Cosmic Rays astrophysics and an upward Neutrino induced air-showering astronomy. Most of this opportunity arises because of neutrino masses, their mixing and the consequent replenishment of rarest tau flavor during its flight in Space. Horizontal air atmosphere act as a filter for High energy Cosmic Rays (CR) and as a beam dump for Ultra High Energy (UHE) neutrinos and a powerfull amplifier for its tau decay in air by its wide showering areas. Earth sharp shadows plays the role of a huge detector volume for UHE neutrino and a noise-free screen for upcoming EeVs tau air-showers (as well PeVs anti-neutrino electron air interactions). Projects for Tau Airshowers are growing at the top of a mountains or at the edge of a cliff. ASHRA in Hawaii and CRNTN in Utah are tracking fluorescence lights, while other novel projects on Crown array detectors on mountains, on balloons and satellites are elaborated for Cherenkov lights. AUGER, facing the Ande edges, ARGO located within a deep valley are testing inclined showers; MILAGRO (and MILAGRITO) may be triggered by horizontal up-going muon bundles from the Earth edges; HIRES and AUGER UHECR detectors, linking twin array telescopes along their axis may test horizontal Cerenkov blazing photons. MAGIC (Hess, Veritas) and Shalon Telescopes may act already like a detector for few PeVs and Glashow resonance neutrino events; MAGIC pointing downward to terrestrial ground acts as a massive tens of km^3 detector, making it the most sensitive dedicated neutrino telescope. MAGIC facing the sea edges must reveal mirrored downward UHECR Air-showers Cherenkov flashes. Magic-crown systems may lead to tens km^3, neutrino detectors.

D. Fargion

2006-04-20T23:59:59.000Z

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181

High-Energy Cosmology: gamma rays and neutrinos from beyond the galaxy  

E-Print Network [OSTI]

Our knowledge of the high-energy universe is undergoing a period of rapid change as new astronomical detectors of high-energy radiation start to operate at their design sensitivities. Now is a boomtime for high-energy astrophysics, with new discoveries from Swift and HESS, results from MAGIC and VERITAS starting to be reported, the upcoming launches of the gamma-ray space telescopes GLAST and AGILE, and anticipated data releases from IceCube and Auger. A formalism for calculating statistical properties of cosmological gamma-ray sources is presented. Application is made to model calculations of the statistical distributions of gamma-ray and neutrino emission from (i) beamed sources, specifically, long-duration GRBs, blazars, and extagalactic microquasars, and (ii) unbeamed sources, including normal galaxies, starburst galaxies and clusters. Expressions for the integrated intensities of faint beamed and unbeamed high-energy radiation sources are also derived. A toy model for the background intensity of radiation from dark-matter annihilation taking place in the early universe is constructed. Estimates for the gamma-ray fluxes of local group galaxies, starburst, and infrared luminous galaxies are briefly reviewed. Because the brightest extragalactic gamma-ray sources are flaring sources, and these are the best targets for sources of PeV -- EeV neutrinos and ultra-high energy cosmic rays, rapidly slewing all-sky telescopes like MAGIC and an all-sky gamma-ray observatory beyond Milagro will be crucial for optimal science return in the multi-messenger age.

Charles D. Dermer

2006-11-06T23:59:59.000Z

182

A General Investigation of Optimized Atmospheric Sample Duration  

SciTech Connect (OSTI)

ABSTRACT The International Monitoring System (IMS) consists of up to 80 aerosol and xenon monitoring systems spaced around the world that have collection systems sensitive enough to detect nuclear releases from underground nuclear tests at great distances (CTBT 1996; CTBTO 2011). Although a few of the IMS radionuclide stations are closer together than 1,000 km (such as the stations in Kuwait and Iran), many of them are 2,000 km or more apart. In the absence of a scientific basis for optimizing the duration of atmospheric sampling, historically scientists used a integration times from 24 hours to 14 days for radionuclides (Thomas et al. 1977). This was entirely adequate in the past because the sources of signals were far away and large, meaning that they were smeared over many days by the time they had travelled 10,000 km. The Fukushima event pointed out the unacceptable delay time (72 hours) between the start of sample acquisition and final data being shipped. A scientific basis for selecting a sample duration time is needed. This report considers plume migration of a nondecaying tracer using archived atmospheric data for 2011 in the HYSPLIT (Draxler and Hess 1998; HYSPLIT 2011) transport model. We present two related results: the temporal duration of the majority of the plume as a function of distance and the behavior of the maximum plume concentration as a function of sample collection duration and distance. The modeled plume behavior can then be combined with external information about sampler design to optimize sample durations in a sampling network.

Eslinger, Paul W.; Miley, Harry S.

2012-11-28T23:59:59.000Z

183

VARIABLE TeV EMISSION AS A MANIFESTATION OF JET FORMATION IN M87?  

SciTech Connect (OSTI)

It is proposed that the variable TeV emission observed in M87 may be produced in a starved magnetospheric region, above which the outflow associated with the VLBA jet is established. It is shown that annihilation of MeV photons emitted by the radiative inefficient flow in the vicinity of the black hole can lead to injection of seed charges on open magnetic field lines, with a density that depends sensitively on accretion rate, n{sub {+-}}{proportional_to} m-dot {sup 4}. For an accretion rate that corresponds to the inferred jet power, and to a fit of the observed spectral energy distribution by an ADAF model, the density of injected pairs is found to be smaller than the Goldreich-Julian (GJ) density by a factor of a few. It is also shown that inverse Compton scattering of ambient photons by electrons (positrons) accelerating in the gap can lead to a large multiplicity, {approx}10{sup 3}, while still allowing photons at energies of up to a few TeV to freely escape the system. The estimated gap width is not smaller than 0.01r{sub s} if the density of seed charges is below the GJ value. The very high energy power radiated by the gap can easily account for the luminosity of the TeV source detected by H.E.S.S. The strong dependence of injected pair density on accretion rate should render the gap emission highly intermittent. We also discuss briefly the application of this mechanism to Sgr A{sup *}.

Levinson, Amir [School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978 (Israel); Rieger, Frank [Max-Planck-Institut fuer Kernphysik, P.O. Box 103980, 69029 Heidelberg (Germany)

2011-04-01T23:59:59.000Z

184

In Wino Veritas? Indirect Searches Shed Light on Neutralino Dark Matter  

E-Print Network [OSTI]

Indirect detection constraints on gamma rays (both continuum and lines) have set strong constraints on wino dark matter. By combining results from Fermi-LAT and HESS, we show that: light nonthermal wino dark matter is strongly excluded; thermal wino dark matter is allowed only if the Milky Way dark matter distribution has a significant (>~0.4 kpc) core; and for plausible NFW and Einasto distributions the entire range of wino masses from 100 GeV up to 3 TeV can be excluded. The case of light, nonthermal wino dark matter is particularly interesting in scenarios with decaying moduli that reheat the universe to a low temperature. Typically such models have been discussed for low reheating temperatures, not far above the BBN bound of a few MeV. We show that constraints on the allowed wino relic density push such models to higher reheating temperatures and hence heavier moduli. Even for a flattened halo model consisting of an NFW profile with constant-density core inside 1 kpc and a density near the sun of 0.3 GeV/cm^3, for 150 GeV winos current data constrains the reheat temperature to be above 1.4 GeV. As a result, for models in which the wino mass is a loop factor below the gravitino mass, the data favor moduli that are more than an order of magnitude heavier than the gravitino. We discuss some of the sobering implications of this result for the status of supersymmetry. We also comment on other neutralino dark matter scenarios, in particular the case of mixed bino/higgsino dark matter. We show that in this case, direct and indirect searches are complementary to each other and could potentially cover most of the parameter space.

JiJi Fan; Matthew Reece

2013-07-16T23:59:59.000Z

185

Accurate Thermochemical Properties for Energetic Materials Applications. I. Heats of Formation of Nitrogen-Containing Heterocycles and Energetic Precursor Molecules from Electronic Structure Theory  

SciTech Connect (OSTI)

The research described in this product was performed in part in the Environmental Molecular Sciences Laboratory, a national scientific user facility sponsored by the Department of Energy's Office of Biological and Environmental Research and located at Pacific Northwest National Laboratory. The heats of formation of 1H-imidazole, 1H-1,2,4-trizazole, 1H-tetrazole, CH3NO2, CH3N3, CH3NH2, CH2- CHNO2, HClO4, and phenol, as well as cations and anions derived from some of the molecules have been calculated using ab initio molecular orbital theory. These molecules are important as models for compounds used for energetic materials synthesis. The predicted heats of formation of the heterocycle-based compounds are in excellent agreement with available experimental values and those derived from proton affinities and deprotonation enthalpies to <1 kcal/mol. The predicted value for the tetrazolium cation differs substantially from the experimental value, likely due to uncertainty in the measurement. The heats of formation of the nitro and amino molecules, as well as phenol/phenolate, also are in good agreement with the experimental values (<1.5 kcal/mol). The heat of formation of CH3N3 is predicted to be 72.8 kcal/mol at 298 K with an estimated error bar of (1 kcal/mol on the basis of the agreement between the calculated and experimental values for ¢Hf(HN3). The heat of formation at 298 K of HClO4 is -0.4 kcal/mol, in very good agreement with the experimental value, as well as a W2 literature study. An extrapolation of the CCSD(T)/aug-cc-pV- (Q,5) energies was required to obtain this agreement. This result suggests that very large basis sets (gaugcc- pV5Z) may be needed to fully recover the valence correlation energy contribution in compounds containing elements with high formal oxidation states at the central atom. In addition tight d functions are needed for the geometry predictions. Douglas-Kroll-Hess (DKH) scalar relativistic corrections for HClO4 and ClO4 - at the MP2 level with correlation-consistent DKH basis sets were predicted to be large, likely due to the high formal oxidation state at the Cl.

Gutowski, Keith E.; Rogers, Robin D.; Dixon, David A.

2006-10-26T23:59:59.000Z

186

Spring Chinook Salmon Oncorhynchus tshawytscha Supplementation in the Clearwater Subbasin ; Nez Perce Tribal Hatchery Monitoring and Evaluation Project, 2007 Annual Report.  

SciTech Connect (OSTI)

The Nez Perce Tribal Hatchery (NPTH) program has the following goals (BPA, et al., 1997): (1) Protect, mitigate, and enhance Clearwater Subbasin anadromous fish resources; (2) Develop, reintroduce, and increase natural spawning populations of salmon within the Clearwater Subbasin; (3) Provide long-term harvest opportunities for Tribal and non-Tribal anglers within Nez Perce Treaty lands within four generations (20 years) following project initiation; (4) Sustain long-term fitness and genetic integrity of targeted fish populations; (5) Keep ecological and genetic impacts to non-target populations within acceptable limits; and (6) Promote Nez Perce Tribal management of Nez Perce Tribal Hatchery Facilities and production areas within Nez Perce Treaty lands. The NPTH program was designed to rear and release 1.4 million fall and 625,000 spring Chinook salmon. Construction of the central incubation and rearing facility NPTH and spring Chinook salmon acclimation facilities were completed in 2003 and the first full term NPTH releases occurred in 2004 (Brood Year 03). Monitoring and evaluation plans (Steward, 1996; Hesse and Cramer, 2000) were established to determine whether the Nez Perce Tribal Hatchery program is achieving its stated goals. The monitoring and evaluation action plan identifies the need for annual data collection and annual reporting. In addition, recurring 5-year program reviews will evaluate emerging trends and aid in the determination of the effectiveness of the NPTH program with recommendations to improve the program's implementation. This report covers the Migratory Year (MY) 2007 period of the NPTH Monitoring & Evaluation (M&E) program. There are three NPTH spring Chinook salmon treatment streams: Lolo Creek, Newsome Creek, and Meadow Creek. In 2007, Lolo Creek received 140,284 Brood Year (BY) 2006 acclimated pre-smolts at an average weight of 34.9 grams per fish, Newsome Creek received 77,317 BY 2006 acclimated pre-smolts at an average of 24.9 grams per fish, and Meadow Creek received 53,425 BY 2006 direct stream release parr at an average of 4.7 grams per fish. Natural and hatchery origin spring Chinook salmon pre-smolt emigrants were monitored from September - November 2006 and smolts from March-June 2007. Data on adult returns were collected from May-September. A suite of performance measures were calculated including total adult and spawner escapement, juvenile production, and survival probabilities. These measures were used to evaluate the effectiveness of supplementation and provide information on the capacity of the natural environment to assimilate and support supplemented salmon populations.

Backman, Thomas; Sprague, Sherman; Bretz, Justin [Nez Perce Tribe

2009-06-10T23:59:59.000Z

187

Synthesis and Evaluation of Cu/SAPO-34 Catalysts for NH3-SCR 2: Solid-state Ion Exchange and One-pot Synthesis  

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Cu-SAPO-34 catalysts are synthesized using two methods: solid-state ion exchange (SSIE) and one-pot synthesis. SSIE is conducted by calcining SAPO-34/CuO mixtures at elevated temperatures. For the one-pot synthesis method, Cu-containing chemicals (CuO and CuSO4) are added during gel preparation. A high-temperature calcination step is also needed for this method. Catalysts are characterized with surface area/pore volume measurements, temperature programmed reduction (TPR), electron paramagnetic resonance (EPR) and nuclear magnetic resonance (NMR) spectroscopies, and scanning electron microscopy (SEM). Catalytic properties are examined using standard ammonia selective catalytic reduction (NH3-SCR) and ammonia oxidation reactions. In Cu-SAPO-34 samples formed using SSIE, Cu presents both as isolated Cu2+ ions and unreacted CuO. The former is highly active and selective in NH3-SCR, while the latter catalyzes a side reaction; notably, the non-selective oxidation of NH3 above 350 ºC. Using the one-pot method followed by a high-temperature aging treatment, it is possible to form Cu SAPO-34 samples with predominately isolated Cu2+ ions at low Cu loadings. However at much higher Cu loadings, isolated Cu2+ ions that bind weakly with the CHA framework and CuO clusters also form. These Cu moieties are very active in catalyzing non-selective NH3 oxidation above 350 ºC. Low-temperature reaction kinetics indicate that Cu-SAPO-34 samples formed using SSIE have core-shell structures where Cu is enriched in the shell layers; while Cu is more evenly distributed within the one-pot samples. Reaction kinetics also suggest that at low temperatures, the local environment next to Cu2+ ion centers plays little role on the overall catalytic properties. The authors gratefully acknowledge the US Department of Energy (DOE), Energy Efficiency and Renewable Energy, Vehicle Technologies Office for the support of this work. The research described in this paper was performed at the Environmental Molecular Sciences Laboratory (EMSL), a national scientific user facility sponsored by the DOE’s Office of Biological and Environmental Research and located at Pacific Northwest National Laboratory (PNNL). PNNL is operated for the US DOE by Battelle under contract number DE-AC05-76RL01830. The authors also thank Shari Li (PNNL) for surface area/pore volume measurements, and Bruce W. Arey (PNNL) for SEM measurements. Discussions with Drs. A. Yezerets, K. Kamasamudram, J.H. Li, N. Currier and J.Y. Luo from Cummins, Inc. and H.Y. Chen and H. Hess from Johnson-Matthey are greatly appreciated.

Gao, Feng; Walter, Eric D.; Washton, Nancy M.; Szanyi, Janos; Peden, Charles HF

2015-01-01T23:59:59.000Z

188

INTERACTING COSMIC RAYS WITH MOLECULAR CLOUDS: A BREMSSTRAHLUNG ORIGIN OF DIFFUSE HIGH-ENERGY EMISSION FROM THE INNER 2 Degree-Sign Multiplication-Sign 1 Degree-Sign OF THE GALACTIC CENTER  

SciTech Connect (OSTI)

The high-energy activity in the inner few degrees of the Galactic center is traced by diffuse radio, X-ray, and {gamma}-ray emission. The physical relationship between different components of diffuse gas emitting at multiple wavelengths is a focus of this work. We first present radio continuum observations using the Green Bank Telescope and model the nonthermal spectrum in terms of a broken power-law distribution of {approx}GeV electrons emitting synchrotron radiation. We show that the emission detected by Fermi is primarily due to nonthermal bremsstrahlung produced by the population of synchrotron emitting electrons in the GeV energy range interacting with neutral gas. The extrapolation of the electron population measured from radio data to low and high energies can also explain the origin of Fe I 6.4 keV line and diffuse TeV emission, as observed with Suzaku, XMM-Newton, Chandra, and the H.E.S.S. observatories. The inferred physical quantities from modeling multiwavelength emission in the context of bremsstrahlung emission from the inner {approx}300 Multiplication-Sign 120 pc of the Galactic center are constrained to have the cosmic-ray ionization rate {approx}1-10 Multiplication-Sign 10{sup -15} s{sup -1}, molecular gas heating rate elevating the gas temperature to 75-200 K, fractional ionization of molecular gas 10{sup -6}-10{sup -5}, large-scale magnetic field 10-20 {mu}G, the density of diffuse and dense molecular gas {approx}100 and {approx}10{sup 3} cm{sup -3} over 300 pc and 50 pc path lengths, and the variability of Fe I K{alpha} 6.4 keV line emission on yearly timescales. Important implications of our study are that GeV electrons emitting in radio can explain the GeV {gamma}-rays detected by Fermi and that the cosmic-ray irradiation model, like the model of the X-ray irradiation triggered by past activity of Sgr A*, can also explain the origin of the variable 6.4 keV emission from Galactic center molecular clouds.

Yusef-Zadeh, F.; Roberts, D. A.; Royster, M. [Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208 (United States)] [Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208 (United States); Hewitt, J. W. [Code 662, NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States)] [Code 662, NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Wardle, M. [Department of Physics and Astronomy, and Research Center for Astronomy, Astrophysics and Astrophotonics, Macquarie University, Sydney, NSW 2109 (Australia)] [Department of Physics and Astronomy, and Research Center for Astronomy, Astrophysics and Astrophotonics, Macquarie University, Sydney, NSW 2109 (Australia); Tatischeff, V. [Center de Spectrometrie Nucleaire et de Spectrometrie de Massse, IN2P3/CNRS and Univ. Paris-Sud, F-91405 Orsay Campus (France)] [Center de Spectrometrie Nucleaire et de Spectrometrie de Massse, IN2P3/CNRS and Univ. Paris-Sud, F-91405 Orsay Campus (France); Cotton, W. [NRAO, 520 Edgemont Road, Charlottesville, VA 22903 (United States)] [NRAO, 520 Edgemont Road, Charlottesville, VA 22903 (United States); Uchiyama, H.; Nobukawa, M.; Tsuru, T. G. [Cosmic Ray Group, Physics, Kyoto University, Kitashirakawa-Oiwake-Cho, Sakyo, Kyoto 606-8502 (Japan)] [Cosmic Ray Group, Physics, Kyoto University, Kitashirakawa-Oiwake-Cho, Sakyo, Kyoto 606-8502 (Japan); Heinke, C. [Department of Physics, Room 238 CEB, University of Alberta, Edmonton, AB T6G 2G7 (Canada)] [Department of Physics, Room 238 CEB, University of Alberta, Edmonton, AB T6G 2G7 (Canada)

2013-01-01T23:59:59.000Z