2014/12/31 by Alexey Tolstov, С. И. Блинников, Sergey Blinnikov +3
Physics and Astronomy · #Accretion (finance) #Active galactic nucleus #Astrophysical Phenomena and Observations #Astrophysical jet #Astrophysics #Classical mechanics #Discontinuity (linguistics) #Galaxy #Gamma-ray bursts and supernovae #Laser-Plasma Interactions and Diagnostics #Mechanics #Physics #Quantum mechanics #Radiative transfer #Shock (circulatory) #Shock wave #Supernova #astro-ph.HE
paper · pdf · doi:10.1088/0004-637x/811/1/47
10 pages, 10 figures, 2 tables, Accepted for publication in Astrophysical Journal, July 23, 2015
openalex publication_date 2015/09/16 · arxiv created 2016/02/29 · arxiv updated 2016/03/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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.