  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.
