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We construct the equation of state (EOS) of nuclear matter at finitetemperature and density with various proton fractions within the relativisticmean field (RMF) theory for the use in the supernova simulations. TheThomas-Fermi approximation is adopted to describe the non-uniform matter wherewe consider nucleus, alpha-particle, proton and neutron in equilibrium. Wetreat the uniform matter and non-uniform matter consistently using the RMFtheory. We tabulate the outcome as the pressure, free energy, entropy etc, withenough mesh points in wide ranges of the temperature, proton fraction, andbaryon mass density.Comment: 22 pages, LaTeX, 9 ps-figures, Submitted to Prog.Theor.Phy

Relativistic Equation of State of Nuclear Matter for Supernova Explosion