Relativistic Equation of State of Nuclear Matter for Supernova Explosion

We construct the equation of state (EOS) of nuclear matter at finite temperature and density with various proton fractions within the relativistic mean field (RMF) theory for the use in the supernova simulations. We consider nucleus, alpha-particle, proton and neutron in equilibrium at densities smaller than about ρB ∼ 1014.2g/cm3 by minimizing the free energy of the nuclear matter. The calculation is based on the RMF theory with the parameter set, TM1, which has been demonstrated to provide good accounts of the ground and the excited state properties of finite nuclei. We tabulate the outcome for various densities as the pressure, the free energy, entropy etc, at enough mesh points in the density range ρB = 105.1 ∼ 1015.4g/cm3 and the temperature range T = 0 ∼ 100MeV and the proton fraction range of Yp = 0 ∼ 0.56 to be used for the supernova simulations. 1

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