Статья

THE AGORA HIGH-RESOLUTION GALAXY SIMULATIONS COMPARISON PROJECT. II. ISOLATED DISK TEST

Ji-hoon KimDepartment of Astronomy, California Institute of Technology, Pasadena, CA 91125, USAOscar AgertzDepartment of Physics, University of Surrey, Guildford, Surrey, GU2 7XH, UKRomain TeyssierCentre for Theoretical Astrophysics and Cosmology, Institute for Computational Science, University of Zurich, Zurich, 8057, SwitzerlandMichael J. ButlerMax-Planck-Institut für Astronomie, D-69117 Heidelberg, GermanyDaniel CeverinoZentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, D-69120 Heidelberg, GermanyJun-Hwan ChoiDepartment of Astronomy, University of Texas, Austin, TX 78712, USARobert FeldmannCentre for Theoretical Astrophysics and Cosmology, Institute for Computational Science, University of Zurich, Zurich, 8057, SwitzerlandBen KellerDepartment of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, CanadaAlessandro LupiInstitut d’Astrophysique de Paris, Sorbonne Universites, UPMC Univ Paris 6 et CNRS, F-75014 Paris, FranceThomas QuinnDepartment of Astronomy, University of Washington, Seattle, WA 98195, USAYves RevazInstitute of Physics, Laboratoire d’Astrophysique, École Polytechnique Fédérale de Lausanne, CH-1015 Lausanne, SwitzerlandSpencer WallaceDepartment of Astronomy, University of Washington, Seattle, WA 98195, USANickolay Y. GnedinDepartment of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USASamuel N. LeitnerDepartment of Astronomy, University of Maryland, College Park, MD 20742, USASijing ShenKavli Institute for Cosmology, University of Cambridge, Cambridge, CB3 0HA, UKBritton D. SmithInstitute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ, UKRobert ThompsonNational Center for Supercomputing Applications, University of Illinois, Urbana, IL 61801, USAMatthew J. TurkSchool of Information Sciences, Department of Astronomy, University of Illinois, Urbana, IL 61801, USATom AbelDepartment of Physics, Stanford University, Stanford, CA 94305, USAKenza S. ArrakiDepartment of Astronomy, New Mexico State University, Las Cruces, NM 88001, USASamantha M. BenincasaDepartment of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, CanadaSukanya ChakrabartiSchool of Physics and Astronomy, Rochester Institute of Technology, Rochester, NY 14623, USAColin DeGrafKavli Institute for Cosmology, University of Cambridge, Cambridge, CB3 0HA, UKAvishai DekelCenter for Astrophysics and Planetary Science, Racah Institute of Physics, The Hebrew University, Jerusalem, 91904, IsraelNathan J. GoldbaumNational Center for Supercomputing Applications, University of Illinois, Urbana, IL 61801, USAPhilip F. HopkinsDepartment of Astronomy, California Institute of Technology, Pasadena, CA 91125, USACameron HummelsDepartment of Astronomy, California Institute of Technology, Pasadena, CA 91125, USAAnatoly KlypinDepartment of Astronomy, New Mexico State University, Las Cruces, NM 88001, USAHui LiDepartment of Astronomy, University of Michigan, Ann Arbor, MI 48109, USAPiero MadauDepartment of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USANir MandelkerCenter for Astrophysics and Planetary Science, Racah Institute of Physics, The Hebrew University, Jerusalem, 91904, IsraelLucio MayerCentre for Theoretical Astrophysics and Cosmology, Institute for Computational Science, University of Zurich, Zurich, 8057, SwitzerlandKentaro NagamineDepartment of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka, 560-0043, JapanSarah NickersonCentre for Theoretical Astrophysics and Cosmology, Institute for Computational Science, University of Zurich, Zurich, 8057, SwitzerlandBrian W. O’SheaDepartment of Computational Mathematics, Science and Engineering, Department of Physics and Astronomy, National Superconducting Cyclotron Laboratory, Michigan State University, Lansing, MI 48824, USAJoel R. PrimackDepartment of Physics, University of California at Santa Cruz, Santa Cruz, CA 95064, USASanti Roca-FàbregaCenter for Astrophysics and Planetary Science, Racah Institute of Physics, The Hebrew University, Jerusalem, 91904, IsraelVadim SemenovDepartment of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USAIkkoh ShimizuDepartment of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka, 560-0043, JapanChristine M. SimpsonHeidelberger Institut für Theoretische Studien, D-69118 Heidelberg, GermanyKeita TodorokiDepartment of Physics and Astronomy, University of Kansas, Lawrence, KS 66045, USAJames W. WadsleyDepartment of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, CanadaJohn WiseCenter for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, Atlanta, GA 30332, USA

2016en

ABI

Аннотация

ABSTRACT Using an isolated Milky Way-mass galaxy simulation, we compare results from nine state-of-the-art gravito-hydrodynamics codes widely used in the numerical community. We utilize the infrastructure we have built for the AGORA High-resolution Galaxy Simulations Comparison Project. This includes the common disk initial conditions, common physics models (e.g., radiative cooling and UV background by the standardized package Grackle ) and common analysis toolkit yt , all of which are publicly available. Subgrid physics models such as Jeans pressure floor, star formation, supernova feedback energy, and metal production are carefully constrained across code platforms. With numerical accuracy that resolves the disk scale height, we find that the codes overall agree well with one another in many dimensions including: gas and stellar surface densities, rotation curves, velocity dispersions, density and temperature distribution functions, disk vertical heights, stellar clumps, star formation rates, and Kennicutt–Schmidt relations. Quantities such as velocity dispersions are very robust (agreement within a few tens of percent at all radii) while measures like newly formed stellar clump mass functions show more significant variation (difference by up to a factor of ∼3). Systematic differences exist, for example, between mesh-based and particle-based codes in the low-density region, and between more diffusive and less diffusive schemes in the high-density tail of the density distribution. Yet intrinsic code differences are generally small compared to the variations in numerical implementations of the common subgrid physics such as supernova feedback. Our experiment reassures that, if adequately designed in accordance with our proposed common parameters, results of a modern high-resolution galaxy formation simulation are more sensitive to input physics than to intrinsic differences in numerical schemes.

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Идентификаторы

DOI: 10.3847/1538-4357/833/2/202

Цитирования и источники

Цитирований: 2Использованных источников: 0

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