  We construct the equation of state (EOS) of nuclear matter using the
relativistic mean field (RMF) theory in the wide density, temperature range
with various proton fractions for the use of supernova simulation and the
neutron star calculations. We first construct the EOS of homogeneous nuclear
matter. We use then the Thomas-Fermi approximation to describe inhomogeneous
matter, where heavy nuclei are formed together with free nucleon gas. We
discuss the results on free energy, pressure and entropy in the wide range of
astrophysical interest. As an example, we apply the resulting EOS on the
neutron star properties by using the Oppenheimer-Volkoff equation.
