Journal
ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
Volume 217, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0067-0049/217/1/9
Keywords
hydrodynamics; line: profiles; methods: numerical; radiation: dynamics; radiative transfer
Categories
Funding
- Department of Energy Office of Science Graduate Fellowship Program (DOE SCGF) [DE-AC05-06OR23100]
- Department of Energy Office of Nuclear Physics Early Career Award [DE-SC0008067]
- Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231, DE-AC05-00OR22725]
- U.S. Department of Energy (DOE) [DE-SC0008067] Funding Source: U.S. Department of Energy (DOE)
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1109896, 1206097] Funding Source: National Science Foundation
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We explore the application of Monte Carlo transport methods to solving coupled radiation-hydrodynamics (RHD) problems. We use a time-dependent, frequency-dependent, three-dimensional radiation transport code that is special relativistic and includes some detailed microphysical interactions such as resonant line scattering. We couple the transport code to two different one-dimensional (non-relativistic) hydrodynamics solvers: a spherical Lagrangian scheme and a Eulerian Godunov solver. The gas-radiation energy coupling is treated implicitly, allowing us to take hydrodynamical time-steps that are much longer than the radiative cooling time. We validate the code and assess its performance using a suite of radiation hydrodynamical test problems, including ones in the radiation energy dominated regime. We also develop techniques that reduce the noise of the Monte Carlo estimated radiation force by using the spatial divergence of the radiation pressure tensor. The results suggest that Monte Carlo techniques hold promise for simulating the multi-dimensional RHD of astrophysical systems.
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