Equations and Algorithms for Mixed-frame Flux-limited Diffusion Radiation Hydrodynamics

By Mark R. Krumholz, Richard Klein, C. McKee, J. Bolstad. 2006

142 citations recorded by the source corpus.

We analyze the mixed-frame equations of radiation hydrodynamics under the approximations of flux-limited diffusion and a thermal radiation field and derive the minimal set of evolution equations that includes all terms that are of leading order in any regime of nonrelativistic radiation hydrodynamics. Our equations are accurate to first order in v/c in the static diffusion regime. In contrast, we show that previous lower order derivations of these equations omit leading terms in at least some regimes. In comparison to comoving-frame formulations of radiation hydrodynamics, our equations have the advantage that they manifestly conserve total energy, making them very well suited to numerical simulations, particularly with adaptive meshes. For systems in the static diffusion regime, our analysis also suggests an algorithm that is both simpler and faster than earlier comoving-frame methods. We implement this algorithm in the Orion adaptive mesh refinement code and show that it performs well in a range of test problems.

Subfields: Computational Mechanics

View Paper: https://www.semanticscholar.org/paper/0e48b36baeb2470873e59c9667bb24813ab67061

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In Computational Mechanics

Citations in the corpus

RADIATION-HYDRODYNAMIC SIMULATIONS OF THE FORMATION OF ORION-LIKE STAR CLUSTERS. II. THE INITIAL MASS FUNCTION FROM WINDS, TURBULENCE, AND RADIATION (2012, methodology): “…whether it be an imposed equation of state (e.g. Bate & Bonnell 2005; Jappsen et al. 2005) or the inclusion of radiative transfer, either without (Bate 2009b, 2012) or with (Krumholz et al. 2007a, 2010, 2011; Offner et al. 2009; Urban et al. 2010) the further step of including stellar radiation.”
THE EFFECTS OF RADIATIVE TRANSFER ON LOW-MASS STAR FORMATION (2009, methodology): “Our code uses the Krumholz et al. (2007b) radiation-hydrodynamic algorithm, in which we split the radiation quantities into those to be handled explicitly and those to be handled implicitly.”
Three-dimensional general relativistic radiation magnetohydrodynamical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure (2013, methodology): “We avoid a fully implicit scheme (e.g., Krumholz et al. 2007; Jiang et al. 2012), which would require us to use a more expensive 8D Newton scheme (to include geometry source terms and expensive multi-cell Riemann flux differences and spatial interpolations within the Newton solver).”
Semi-implicit scheme for treating radiation under M1 closure in general relativistic conservative fluid dynamics codes (2012, methodology): “In principle, we could try to solve the whole system of partial differential equations (23)–(25) implicitly, as done for instance in non-relativistic or special relativistic radiation hydrodynamics codes (e.g. Krumholz et al. 2007; Jiang et al. 2012).”
ramses-rt: radiation hydrodynamics in the cosmological context (2013, methodology): “The FLD method has been used by e.g. Krumholz et al. (2007), Reynolds et al. (2009) and Commerçon et al. (2011), mainly for the purpose of studying the momentum feedback of infrared radiation on to dusty and optically thick gas, rather than photoionization of hydrogen and helium.”
DIRECT NUMERICAL SIMULATION OF RADIATION PRESSURE-DRIVEN TURBULENCE AND WINDS IN STAR CLUSTERS AND GALACTIC DISKS (2012, methodology): “The code uses the conservative operator-splitting scheme of Krumholz et al. (2007) to separate the implicit radiation and explicit hydrodynamic updates.”
yt: A MULTI-CODE ANALYSIS TOOLKIT FOR ASTROPHYSICAL SIMULATION DATA (2010, background): “…underlying representation of state variables have enabled it to be extended to work with a number of other simulation codes natively, including Orion (Truelove et al. 1998; Klein et al. 1999; Krumholz et al. 2004, 2007), FLASH (Fryxell et al. 2000), Chombo (LLNL 2010) and RAMSES (Teyssier 2002).”
H II REGIONS: WITNESSES TO MASSIVE STAR FORMATION (2010, methodology): “Krumholz et al. (2007b) initialized a microturbulent flow within their dense core, but Krumholz et al. (2009b) found that it made little difference by the time material had collapsed to the size of the disk.”