Equations and Algorithms for Mixed Frame Flux-Limited Diffusion Radiation Hydrodynamics
arXiv:astro-ph/0611003 · doi:10.1086/520791
Abstract
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 non-relativistic 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.
19 pages, 12 figures, emulateapj format, accepted to ApJS. This version contains additional code verification tests and some changes to the discussion. The basic results derived are unchanged
References in corpus (11)
- Radiation Pressure Supported Starburst Disks and AGN Fueling
- Radiation-Hydrodynamic Simulations of Collapse and Fragmentation in Massive Protostellar Cores
- Simulating Radiating and Magnetized Flows in Multi-Dimensions with ZEUS-MP
- Embedding Lagrangian Sink Particles in Eulerian Grids
- A Module for Radiation Hydrodynamic Calculations With ZEUS-2D Using Flux-Limited Diffusion
- How Protostellar Outflows Help Massive Stars Form
- A faster algorithm for smoothed particle hydrodynamics with radiative transfer in the flux-limited diffusion approximation
- Local Three-Dimensional Simulations of Magneto-Rotational Instability in Radiation-Dominated Accretion Disks
- Smoothed particle hydrodynamics with radiative transfer in the flux-limited diffusion approximation
- A New Algorithm for 2-D Transport for Astrophysical Simulations: I. General Formulation and Tests for the 1-D Spherical Case
- A Modified Higher Order Godunov's Scheme for Stiff Source Conservative Hydrodynamics
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- CASTRO: A New Compressible Astrophysical Solver. II. Gray Radiation Hydrodynamics
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