  Temperature dependence of an electron-nuclear plasma equilibrium density is
considered basing on known approaches, which are given in (1)(2). It is shown
that at a very high temperature, which is characteristic for a star interior,
the equilibrium plasma density is almost constant and equals approximately to
$10^{25}$ particles per $cm^3$. At a relatively low temperature, which is
characteristic for star surface, the equilibrium plasma density is in several
orders lower and depends on temperature as $T^{3/2}$.
