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Title:
Cosmological radiative transfer comparison project - II. The radiation-hydrodynamic tests
Authors:
Iliev, Ilian T.; Whalen, Daniel; Mellema, Garrelt; Ahn, Kyungjin; Baek, Sunghye; Gnedin, Nickolay Y.; Kravtsov, Andrey V.; Norman, Michael; Raicevic, Milan; Reynolds, Daniel R.; Sato, Daisuke; Shapiro, Paul R.; Semelin, Benoit; Smidt, Joseph; Susa, Hajime; Theuns, Tom; Umemura, Masayuki
Affiliation:
AA(Astronomy Centre, Department of Physics & Astronomy, Pevensey II Building, University of Sussex, Falmer, Brighton BN1 9QH; Universität Zürich, Institut für Theoretische Physik, Winterthurerstrasse 190, CH-8057 Zürich, Switzerland; Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada), AB(T-2 Nuclear and Particle Physics, Astrophysics, and Cosmology, Los Alamos National Laboratory, Los Alamos, NM 87545, USA), AC(Department of Astronomy and Oskar Klein Centre, AlbaNova, Stockholm University, SE-10691 Stockholm, Sweden), AD(Department of Earth Science Education, Chosun University, Gwangju 501-759, Korea; Department of Astronomy, University of Texas, Austin, TX 78712-1083, USA), AE(LERMA, Observatoire de Paris & UPMC, 77 av Denfert Rochereau, 75014 Paris, France), AF(Fermilab, MS209, P.O. 500, Batavia, IL 60510, USA), AG(Department of Astronomy and Astrophysics, Center for Cosmological Physics, The University of Chicago, Chicago, IL 60637, USA), AH(Center for Astrophysics and Space Sciences, University of California, San Diego, 9500 Gilman Drive, La Jolla, CA 92093-0424, USA), AI(Institute for Computational Cosmology, Durham University, Durham DH1 3LE), AJ(Department of Mathematics, 208 Clements Hall, Southern Methodist University, Dallas, TX 75275, USA), AK(Center for Computational Sciences, University of Tsukuba, Tsukuba, Ibaraki 305-8577, Japan), AL(Department of Astronomy, University of Texas, Austin, TX 78712-1083, USA), AM(LERMA, Observatoire de Paris & UPMC, 77 av Denfert Rochereau, 75014 Paris, France), AN(Department of Physics and Astronomy, 4129 Frederick Reines Hall, UC Irvine, Irvine, CA 84602, USA), AO(Department of Physics, Konan University, Kobe, Japan), AP(Institute for Computational Cosmology, Durham University, Durham DH1 3LE; Department of Physics, University of Antwerp, Campus Groenenborger, Groenenborgerlaan B-171, B2020 Antwerp, Belgium), AQ(Center for Computational Sciences, University of Tsukuba, Tsukuba, Ibaraki 305-8577, Japan)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 400, Issue 3, pp. 1283-1316. (MNRAS Homepage)
Publication Date:
12/2009
Origin:
MNRAS
MNRAS Keywords:
radiative transfer , methods: numerical , HII regions , galaxies: high-redshift , intergalactic medium , cosmology: theory
Abstract Copyright:
(c) Journal compilation © 2009 RAS
DOI:
10.1111/j.1365-2966.2009.15558.x
Bibliographic Code:
2009MNRAS.400.1283I

Abstract

The development of radiation hydrodynamical methods that are able to follow gas dynamics and radiative transfer (RT) self-consistently is key to the solution of many problems in numerical astrophysics. Such fluid flows are highly complex, rarely allowing even for approximate analytical solutions against which numerical codes can be tested. An alternative validation procedure is to compare different methods against each other on common problems, in order to assess the robustness of the results and establish a range of validity for the methods. Previously, we presented such a comparison for a set of pure RT tests (i.e. for fixed, non-evolving density fields). This is the second paper of the Cosmological Radiative Transfer Comparison Project, in which we compare nine independent RT codes directly coupled to gas dynamics on three relatively simple astrophysical hydrodynamics problems: (i) the expansion of an HII region in a uniform medium, (ii) an ionization front in a 1/r2 density profile with a flat core and (iii) the photoevaporation of a uniform dense clump. Results show a broad agreement between the different methods and no big failures, indicating that the participating codes have reached a certain level of maturity and reliability. However, many details still do differ, and virtually every code has showed some shortcomings and has disagreed, in one respect or another, with the majority of the results. This underscores the fact that no method is universal and all require careful testing of the particular features which are most relevant to the specific problem at hand.
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