Extended relativistic non-equilibrium thermostatics of stellar structures with radiation pressure. (arXiv:2106.00408v2 [gr-qc] UPDATED)
<a href="http://arxiv.org/find/gr-qc/1/au:+Balakin_A/0/1/0/all/0/1">Alexander B. Balakin</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Tukbaev_Z/0/1/0/all/0/1">Zagir Z. Tukbaev</a>
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.
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.
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