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arXiv · 1412.1434

Shock wave structure in astrophysical flows with an account of photon transfer

Alexey Tolstov·Sergey Blinnikov·Shigehiro Nagataki·Ken'ichi Nomoto
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Abstract

For an accurate treatment of the shock wave propagation in high-energy astrophysical phenomena, such as supernova shock breakouts, gamma-ray bursts and accretion disks, knowledge of radiative transfer plays a crucial role. In this paper we consider one-dimensional (1D) special relativistic radiation hydrodynamics by solving the Boltzmann equation for radiative transfer. The structure of a radiative shock is calculated for a number of shock tube problems, including strong shock waves, and relativistic- and radiation-dominated cases. Calculations are performed using an iterative technique that consistently solves the equations of relativistic hydrodynamics and relativistic comoving radiative transfer. A comparison of radiative transfer solutions with the Eddington approximation and the M1 closure is made. A qualitative analysis of moment equations for radiation is performed and the conditions for the existence of jump discontinuity for non-relativistic cases are investigated numerically.

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Alexey Tolstov, Sergey Blinnikov, Shigehiro Nagataki, Ken'ichi Nomoto. 2014-12-03. Shock wave structure in astrophysical flows with an account of photon transfer. https://doi.org/10.1088/0004-637x%2F811%2F1%2F47

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