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Planck intermediate results. LVI. Detection of the CMB dipole through modulation of the thermal Sunyaev-Zeldovich effect: Eppur si muove II

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arXiv 2020年

作者： Akrami, Y. Ashdown, M. Baccigalupi, C. Ballardini, M. Banday, A.J. Barreiro, R.B. Bartolo, N. Basak, S. Benabed, K. Bernard, J.-P. Bersanelli, M. Bielewicz, P. Bond, J.R. Borrill, J. Burigana, C. Calabrese, E. Cardoso, J.-F. Casaponsa, B. Chiang, H.C. Combet, C. Contreras, D. Crill, B.P. Cuttaia, F. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Di Valentino, E. Diego, J.M. Doré, O. Douspis, M. Dupac, X. Enßlin, T.A. Eriksen, H.K. Fernandez-Cobos, R. Finelli, F. Frailis, M. Franceschi, E. Frolov, A. Galeotta, S. Galli, S. Ganga, K. Génova-Santos, R.T. Gerbino, M. González-Nuevo, J. Górski, K.M. Gruppuso, A. Gudmundsson, J.E. Handley, W. Herranz, D. Hivon, E. Huang, Z. Jaffe, A.H. Jones, W.C. Keihänen, E. Keskitalo, R. Kiiveri, K. Kim, J. Kisner, T.S. Krachmalnicoff, N. Kunz, M. Kurki-Suonio, H. Lamarre, J.-M. Lattanzi, M. Lawrence, C.R. Le Jeune, M. Levrier, F. Liguori, M. Lilje, P.B. Lindholm, V. López-Caniego, M. Macías-Pérez, J.F. Maino, D. Mandolesi, N. Marcos-Caballero, A. Maris, M. Martin, P.G. Martínez-González, E. Matarrese, S. Mauri, N. McEwen, J.D. Mennella, A. Migliaccio, M. Molinari, D. Moneti, A. Montier, L. Morgante, G. Moss, A. Natoli, P. Pagano, L. Paoletti, D. Perrotta, F. Pettorino, V. Piacentini, F. Polenta, G. Rachen, J.P. Reinecke, M. Remazeilles, M. Renzi, A. Rocha, G. Rosset, C. Rubiño-Martín, J.A. Ruiz-Granados, B. Salvati, L. Savelainen, M. Scott, D. Sirignano, C. Sirri, G. Spencer, L.D. Sunyaev, R. Suur-Uski, A.-S. Tauber, J.A. Tavagnacco, D. Tenti, M. Toffolatti, L. Tomasi, M. Trombetti, T. Valiviita, J. van Tent, B. Vielva, P. Villa, F. Vittorio, N. Wehus, I.K. Zacchei, A. Zonca, A. AIM CEA CNRS Université Paris-Saclay Université Paris-Diderot Sorbonne Paris Cité Gif-sur-YvetteF-91191 France APC AstroParticule et Cosmologie Université Paris Diderot CNRS IN2P3 CEA Lrfu Observatoire de Paris Sorbonne Paris Cité 10 rue Alice Domon et Léonie Duquet Paris Cedex 1375205 France African Institute for Mathematical Sciences 6-8 Melrose Road Muizenberg Cape Town South Africa Astrophysics Group Cavendish Laboratory University of Cambridge J J Thomson Avenue CambridgeCB3 0HE United Kingdom Astrophysics & Cosmology Research Unit School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Private Bag X54001 Durban4000 South Africa CITA University of Toronto 60 St. George St. TorontoONM5S 3H8 Canada CNRS IRAP 9 Av. colonel Roche BP 44346 Toulouse Cedex 4F-31028 France California Institute of Technology PasadenaCA United States Computational Cosmology Center Lawrence Berkeley National Laboratory BerkeleyCA United States Département de Physique Théorique Université de Genève 24 Quai E. Ansermet Genève 41211 Switzerland Département de Physique École normale supérieure PSL Research University CNRS 24 rue Lhomond Paris75005 France La Laguna TenerifeE-38206 Spain Departamento de Física Universidad de Oviedo C/ Federico García Lorca 18 Oviedo Spain Department of Astrophysics IMAPP Radboud University P.O. Box 9010 Nijmegen6500 GL Netherlands Department of Physics & Astronomy University of British Columbia 6224 Agricultural Road VancouverBC Canada Department of Physics & Astronomy University of the Western Cape Cape Town7535 South Africa Department of Physics and Astronomy York University TorontoONM3J 1P3 Canada Department of Physics Gustaf Hällströmin katu 2a University of Helsinki Helsinki Finland Department of Physics Princeton University PrincetonNJ United States Dipartimento di Fisica e Astronomia G. Galilei Università degli Studi di Padova via Marzolo 8 Padova351

The largest temperature anisotropy in the cosmic microwave background (CMB) is the dipole, which has been measured with increasing accuracy for more than three decades, particularly with the Planck satellite. The simplest interpretation of the dipole is that it is due to our motion with respect to the rest frame of the CMB. Since current CMB experiments infer temperature anisotropies from angular intensity variations, the dipole modulates the temperature anisotropies with the same frequency dependence as the thermal Sunyaev-Zeldovich (tSZ) effect. We present the first (and significant) detection of this signal in the tSZ maps, and find that it is consistent with direct measurements of the CMB dipole, as expected. The signal contributes power in the tSZ maps, modulated in a quadrupolar pattern, and we estimate its contribution to the tSZ bispectrum, noting that it contributes negligible noise to the bispectrum at relevant scales. Copyright © 2020, The Authors. All rights reserved.

关键词： Cosmology

High-Girth matrices and polarization

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High-Girth matrices and polarization

IEEE International Symposium on Information Theory

作者： Emmanuel Abbe Yuval Wigderson Prog. in Applied and Computational Math Princeton University Department of Mathematics Princeton University

ISBN: (纸本)9781467377058

The girth of a matrix is the least number of linearly dependent columns, in contrast to the rank which is the largest number of linearly independent columns. This paper considers the construction of high-girth matrices, whose probabilistic girth is close to their rank. Random matrices can be used to show the existence of high-girth matrices. This paper uses a recursive construction based on conditional ranks (inspired by polar codes) to obtain a deterministic and efficient construction of high-girth matrices for arbitrary relative ranks. Interestingly, the construction is agnostic to the underlying field and applies to both finite and continuous fields with the same binary matrix. The construction gives in particular the following: (i) over the binary field, high-girth matrices are equivalent to capacity-achieving codes, and our construction turns out to match exactly the BEC polar codes (even at finite block length). It hence gives a different interpretation of BEC polar codes, using the parity-check matrix instead of the generator matrix, and basic linear algebra instead of the mutual information, and generalizes to larger fields; (ii) for the BSC, our construction gives an operational meaning to the Bhattacharyya upper-bound process used in polar codes; (iii) for the reals, it gives an explicit candidate matrix for sparse recovery.

关键词： Probabilistic logic Sparse matrices Linear codes Decoding Mutual information Parity check codes

Real-space investigation of short-range magnetic correlations in uoride pyrochlores NaCaCo2F7 and NaSrCo2F7 with magnetic pair distribution function analysis

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arXiv 2017年

作者： Frandsen, Benjamin A. Ross, Kate A. Krizan, Jason W. Nilsen, Goran J. Wildes, Andrew R. Cava, Robert J. Birgeneau, Robert J. Billinge, Simon J.L. Materials Sciences Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics University of California BerkeleyCA94720 United States Department of Physics Colorado State University Fort CollinsCO80523 United States Quantum Materials Program Canadian Institute for Advanced Research TorontoONM5G1Z8 Canada Department of Physics Princeton University PrincetonNJ08544 United States Institut Laue-Langevin CS 20156 Grenoble Cedex 938042 France ISIS Neutron and Muon Facility Rutherford Appleton Laboratory DidcotOX110QX United Kingdom Institut Laue-Langevin Grenoble38000 France Materials Science Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Materials Science and Engineering University of California BerkeleyCA94720 United States Condensed Matter Physics and Materials Science Department Brookhaven National Laboratory UptonNY11973 United States Department of Applied Physics and Applied Mathematics Columbia University New YorkNY10027 United States

We present time-of-ight neutron total scattering and polarized neutron scattering measurements of the magnetically frustrated compounds NaCaCo2F7 and NaSrCo2F7, which belong to a class of recently discovered pyrochlore compounds based on transition metals and uorine. The magnetic pair distribution function (mPDF) technique is used to analyze and model the total scattering data in real space. We find that a previously-proposed model of short-range XY-like correlations with a length scale of 10-15 A, combined with nearest-neighbor collinear antiferromagnetic correlations, accurately describes the mPDF data at low temperature, confirming the magnetic ground state in these materials. This model is further verified by the polarized neutron scattering data. From an analysis of the temperature dependence of the mPDF and polarized neutron scattering data, we find that short-range correlations persist on the nearest-neighbor length scale up to 200 K, approximately two orders of magnitude higher than the spin freezing temperatures of these compounds. These results highlight the opportunity presented by these new pyrochlore compounds to study the effects of geometric frustration at relatively high temperatures, while also advancing the mPDF technique and providing a novel opportunity to investigate a genuinely short-range-ordered magnetic ground state directly in real space. Copyright © 2017, The Authors. All rights reserved.

关键词： Magnetism

Pseudo prolate spheroidal functions

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Pseudo prolate spheroidal functions

International Conference on Sampling Theory and Applications (SampTA)

作者： Luís Daniel Abreu João M. Pereira Austrian Academy of Sciences Acoustics Research Institute Vienna Austria Program in Applied and Computational Mathematics Princeton University Princeton NJ USA

Let Dt and B Ω denote the operators which cut the time content outside T and the frequency content outside Ω, respectively. The prolate spheroidal functions are the eigen-functions of the operator Pτ, Ω = D t B Ω D t . With the aim of formulating in precise mathematical terms the notion of Nyquist rate, Landau and Pollack have shown that, asymptotically, the number of such functions with eigenvalue close to one is ≈ |T||Ω|/2π. We have recently revisited this problem with a new approach: instead of counting the number of eigenfunctions with eigenvalue close to one, we count the maximum number of orthogonal ε-pseudoeigenfunctions with ε-pseudoeigenvalue one. Precisely, we count how many orthogonal functions have a maximum of energy e outside the domain T x Ω, in the sense that ||P T, Ω f - f|| 2 ≤ ε. We have recently discovered that the sharp asymptotic number is ≈ (1 - ε) -1 |T||Ω|/2π. The proof involves an explicit construction of the pseudoeigenfunctions of P T, Ω . When T and Ω are intervals we call them pseudo prolate spheroidal functions. In this paper we explain how they are constructed.

关键词： Eigenvalues and eigenfunctions Time-frequency analysis Fourier transforms Linear approximation

Fundamental physics with the square kilometre array

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arXiv 2018年

作者： Weltman, A. Bull, P. Camera, S. Kelley, K. Padmanabhan, H. Pritchard, J. Racanelli, A. Riemer-Sørensen, S. Shao, L. Andrianomena, S. Athanassoula, E. Bacon, D. Barkana, R. Bertone, G. Bonvin, C. Bosma, A. Brüggen, M. Burigana, C. Bœhm, C. Calore, F. Cembranos, J.A.R. Clarkson, C. Connors, R.M.T. de la Cruz-Dombriz, Á. Dunsby, P.K.S. Fonseca, J. Fornengo, N. Gaggero, D. Harrison, I. Larena, J. Ma, Y.-Z. Maartens, R. Méndez-Isla, M. Mohanty, S.D. Murray, S.G. Parkinson, D. Pourtsidou, A. Quinn, P. Regis, M. Saha, P. Sahlén, M. Sakellariadou, M. Silk, J. Trombetti, T. Vazza, F. Venumadhav, T. Vidotto, F. Villaescusa-Navarro, F. Wang, Y. Weniger, C. Wolz, L. Zhang, F. Gaensler, B.M. Department of Mathematics & Applied Mathematics University of Cape Town 7701 Rondebosch Cape Town South Africa Department of Astronomy University of California Berkeley BerkeleyCA94720 United States Dipartimento di Fisica Università degli Studi di Torino INFN Sezione di Torino INAF – Istituto Nazionale di Astrofisica Via P. Giuria 1 Torino10125 Italy University of Western Australia Ken and Julie Michael Building 7 Fairway CrawleyWA6009 Australia ETH Zurich Wolfgang-Pauli-Strasse 27 ZurichCH 8093 Switzerland Department of Physics Imperial College London Prince Consort Road LondonSW7 2AZ United Kingdom Martí Franquès 1 BarcelonaE08028 Spain Institute of Theoretical Astrophysics University of Oslo P.O. Box 1029 Blindern OsloN-0315 Norway Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China The Park Park Road Cape Town7405 South Africa Aix Marseille Univ CNRS CNES LAM Marseille France Institute of Cosmology & Gravitation University of Portsmouth PortsmouthPO1 3FX United Kingdom Raymond and Beverly Sackler School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel GRAPPA Institute of Physics University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands School of Physics University of Sydney NSW Australia 2006 Australia Département de Physique Théorique Center for Astroparticle Physics Université de Genève Genève 41211 Switzerland Aix Marseille Univ CNRS CNES LAM Marseille France University of Hamburg Gojenbergsweg 112 Hamburg21029 Germany INAF Istituto di Radioastronomia Via Piero Gobetti 101 BolognaI-40129 Italy GRAPPA Institute of Physics University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands Departamento de Física Teórica I and UPARCOS Universidad Complutense de Madrid MadridE-28040 Spain School of Physics & Astronomy Queen Mary University of London LondonE1 4NS United Kingdom Cahill Center for Astronomy and Astrophysics California Instit

The Square Kilometre Array (SKA) is a planned large radio interferometer designed to operate over a wide range of frequencies, and with an order of magnitude greater sensitivity and survey speed than any current radio telescope. The SKA will address many important topics in astronomy, ranging from planet formation to distant galaxies. However, in this work, we consider the perspective of the SKA as a facility for studying physics. We review four areas in which the SKA is expected to make major contributions to our understanding of fundamental physics: cosmic dawn and reionisation;gravity and gravitational radiation;cosmology and dark energy;and dark matter and astroparticle physics. These discussions demonstrate that the SKA will be a spectacular physics machine, which will provide many new breakthroughs and novel insights on matter, energy and spacetime. Copyright © 2018, The Authors. All rights reserved.

关键词： Galaxies

THE SIMONS OBSERVATORY: SCIENCE GOALS AND FORECASTS

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arXiv 2018年

作者： Ade, Peter Aguirre, James Ahmed, Zeeshan Aiola, Simone Ali, Aamir Alonso, David Alvarez, Marcelo A. Arnold, Kam Ashton, Peter Austermann, Jason Awan, Humna Baccigalupi, Carlo Baildon, Taylor Barron, Darcy Battaglia, Nick Battye, Richard Baxter, Eric Bazarko, Andrew Beall, James A. Bean, Rachel Beck, Dominic Beckman, Shawn Beringue, Benjamin Bianchini, Federico Boada, Steven Boettger, David Bond, J. Richard Borrill, Julian Brown, Michael L. Bruno, Sarah Marie Bryan, Sean Calabrese, Erminia Calafut, Victoria Calisse, Paolo Carron, Julien Challinor, Anthony Chesmore, Grace Chinone, Yuji Chluba, Jens Cho, Hsiao-Mei Sherry Choi, Steve Coppi, Gabriele Cothard, Nicholas F. Coughlin, Kevin Crichton, Devin Crowley, Kevin D. Crowley, Kevin T. Cukierman, Ari D’Ewart, John M. Dünner, Rolando de Haan, Tijmen Devlin, Mark Dicker, Simon Didier, Joy Dobbs, Matt Dober, Bradley Duell, Cody J. Duff, Shannon Duivenvoorden, Adri Dunkley, Jo Dusatko, John Errard, Josquin Fabbian, Giulio Feeney, Stephen Ferraro, Simone Fluxà, Pedro Freese, Katherine Frisch, Josef C. Frolov, Andrei Fuller, George Fuzia, Brittany Galitzki, Nicholas Gallardo, Patricio A. Ghersi, Jose Tomas Galvez Gao, Jiansong Gawiser, Eric Gerbino, Martina Gluscevic, Vera Goeckner-Wald, Neil Golec, Joseph Gordon, Sam Gralla, Megan Green, Daniel Grigorian, Arpi Groh, John Groppi, Chris Guan, Yilun Gudmundsson, Jon E. Han, Dongwon Hargrave, Peter Hasegawa, Masaya Hasselfield, Matthew Hattori, Makoto Haynes, Victor Hazumi, Masashi He, Yizhou Healy, Erin Henderson, Shawn W. Hervias-Caimapo, Carlos Hill, Charles A. Hill, J. Colin Hilton, Gene Hilton, Matt Hincks, Adam D. Hinshaw, Gary Hložek, Renée Ho, Shirley Ho, Shuay-Pwu Patty Howe, Logan Huang, Zhiqi Hubmayr, Johannes Huffenberger, Kevin Hughes, John P. Ijjas, Anna Ikape, Margaret Irwin, Kent Jaffe, Andrew H. Jain, Bhuvnesh Jeong, Oliver Kaneko, Daisuke Karpel, Ethan D. Katayama, Nobuhiko Keating, Brian Kernasovskiy, Sarah S. Keskitalo, Reijo Kisner, Theodore Kiuchi, Kenji Klein, Jeff Knowles, Kenda Koopman, Brian Kosowsk School of Physics and Astronomy Cardiff University The Parade CardiffCF24 3AA United Kingdom Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States Kavli Institute for Particle Astrophysics and Cosmology Menlo ParkCA94025 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Joseph Henry Laboratories of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Department of Physics University of California BerkeleyCA94720 United States University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom Computational Cosmology Center Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics University of California San Diego CA92093 United States Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States University of Tokyo Kashiwa277- 8583 Japan NIST Quantum Sensors Group 325 Broadway Mailcode 687.08 BoulderCO80305 United States Department of Physics and Astronomy Rutgers State University of New Jersey PiscatawayNJ08854-8019 United States Via Bonomea 265 Trieste34136 Italy INFN Sezione di Trieste Padriciano 99 Trieste34149 Italy Department of Physics University of Michigan Ann Arbor48103 United States Department of Physics and Astronomy University of New Mexico AlbuquerqueNM87131 United States Department of Astronomy Cornell University IthacaNY14853 United States Jodrell Bank Centre for Astrophysics School of Physics and Astronomy University of Manchester Manchester United Kingdom AstroParticule et Cosmologie Univ Paris Diderot CNRS/IN2P3 CEA/Irfu Obs de Paris Sorbonne Paris Cité France DAMTP Centre for Mathematical Sciences University of Cambridge Wilberforce Road CambridgeCB3 OWA United Kingdom School of Physics Universi

The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping ≈ 10% of the sky to a white noise level of 2 µK-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of σ(r) = 0.003. The large aperture telescope will map ≈ 40% of the sky at arcminute angular resolution to an expected white noise level of 6 µK-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev–Zel’dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sou

关键词： Tensors

Single-point kinetic energy density functionals: A pointwise kinetic energy density analysis and numerical convergence investigation

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Physical Review B 2015年第4期91卷 045124-045124页

作者： Junchao Xia Emily A. Carter Department of Mechanical and Aerospace Engineering Princeton University Princeton New Jersey 08544-5263 USA Program in Applied and Computational Mathematics and Andlinger Center for Energy and the Environment Princeton University Princeton New Jersey 08544-5263 USA

We present a comprehensive study of single-point kinetic energy density functionals (KEDFs) to be used in orbital-free density functional theory (DFT) calculations. We first propose a form of KEDFs based on a pointwise Kohn-Sham (KS) kinetic energy density (KED) and electron localization function (ELF) analysis. We find that the ELF and modified enhancement factor have a very strong and transferable correlation with the reduced density in various bulk metals. The non-self-consistent kinetic energy errors predicted by our KEDF models are decreased greatly compared to previously reported generalized gradient approximation (GGA) KEDFs. Second, we perform self-consistent calculations with various single-point KEDFs and investigate their numerical convergence behavior. We find striking numerical instabilities for previous GGA KEDFs; most of the GGA KEDFs fail to converge and show unphysical densities during the optimization. In contrast, our KEDFs demonstrate stable convergence, and their self-consistent results of various bulk properties agree reasonably well with KSDFT. A further detailed KED analysis reveals an interesting bifurcation phenomenon in defective metals and alloys, which may shed light on directions for future KEDF development.

关键词： KINETIC energy DENSITY functionals DENSITY functional theory ELECTRON research BIFURCATION theory

Reply to “Comment on ‘Single-point kinetic energy density functionals: A pointwise kinetic energy density analysis and numerical convergence investigation’ ”

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Physical Review B 2015年第11期92卷 117102-117102页

We find that the multivalued character of the G factor as a function of the reduced gradient (s) still exists after accounting for pseudopotential artifacts and the kinetic energy global upper bound. We also find that the VT84F functional indeed exhibits stable convergence and more reasonable results for self-consistent bulk properties compared to other generalized gradient approximation (GGA) kinetic energy density functionals (KEDFs) that we tested earlier. However, VT84F generally yields overestimated equilibrium volumes, which may result from its inability (as with all GGAs) to reproduce the G−s multivalued character. The analogous failure to predict the multivalued character of G as a function of the reduced density (d) is also likely to be responsible for the inaccuracy of our vWGTF functionals reported earlier. Our multivaluedness analysis therefore does not impugn any particular GGA KEDF. Instead, it merely confirms the importance of pointwise analysis for improving KEDFs by emphasizing the need to resolve the multivaluedness of G with respect to various density variables.

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Outcomes from the DOE workshop on turbulent flow simulation at the exascale 46

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Outcomes from the DOE workshop on turbulent flow simulation ...

46th AIAA Fluid Dynamics Conference, 2016

作者： Sprague, Michael A. Boldyrev, Stanislav Chang, Choong-Seock Fischer, Paul Grout, Ray Gustafson, William I. Hittinger, Jeffrey A. F. Merzari, Elia Moser, Robert National Renewable Energy Laboratory 15013 DenverWest Parkway GoldenCO80401 United States University of Wisconsin-Madison MadisonWI53706 United States Princeton University PrincetonNJ08543 United States University of Illinois at Urbana-Champaign UrbanaIL61801 United States National Renewable Energy Laboratory GoldenCO80401 United States Pacific Northwest National Laboratory RichlandWA99352 United States Lawrence Livermore National Laboratory LivermoreCA94551 United States Argonne National Laboratory ArgonneIL60439 United States University of Texas at Austin AustinTX78712 United States Computational Science Center 15013 DenverWest Parkway United States Physics Department 1150 University Avenue United States Princeton Plasma Physics Laboratory P.O. Box 451 United States Department of Computer Science 201 North Goodwin Avenue United States Computational Science Center 5013 Denver West Parkway United States Atmospheric Sciences and Global Change Division P.O. Box 999 K9-30 United States Scientific Computing Group Center for Applied Scientific Computing PO Box 808 L-561 United States Mathematics and Computer Science 9700 S. Cass Avenue United States Institute for Computational Engineering and Sciences and Department of Mechanical Engineering 201 East 24th United States

ISBN: (数字)9781624104367

ISBN: (纸本)9781624104367

This paper summarizes the outcomes from the Turbulent Flow Simulation at the Exascale: Opportunities and Challenges Workshop, which was held 4-5 August 2015, and was sponsored by the U.S. Department of Energy (DOE) Office of Advanced Scientific Computing Research (ASCR). The workshop objectives were to define and describe the challenges and opportunities that computing at the exascale will bring to turbulent-flow simulations in applied science and technology. The need for accurate simulation of turbulent flows is evident across the DOE applied-science and engineering portfolios, including combustion, plasma physics, nuclear-reactor physics, wind energy, and atmospheric science. The work-shop brought together experts in turbulent-flow simulation, computational mathematics, and high-performance computing. Building upon previous ASCR workshops on exascale computing, participants defined a research agenda and path forward that will enable scientists and engineers to continually leverage, engage, and direct advances in computational systems on the path to exascale computing. © 2016, American Institute of Aeronautics and Astronautics Inc, AIAA. All rights reserved.

关键词： Turbulent flow