Extended relativistic non-equilibrium thermostatics of stellar
  structures with radiation pressure
  We establish the extended formalism for description of the static spherically
symmetric relativistic non-equilibrium stellar systems in the formation of
which the radiation pressure plays the key role. The main concept of this
extended formalism inherits the ideas, on which the Israel-Stewart causal
thermodynamics is based, but now the unit spacelike four-vector, indicated by
the term director, is exploited in addition to the unit timelike medium
velocity four-vector. An application of the extended formalism is considered;
we analyze the profiles of the non-equilibrium pressure and temperature as the
functions of guiding parameters introduced phenomenologically.
