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 use in supernova simulations. We consider nuclei, alpha-particles, protons and neutrons in equilibrium at densities smaller than about ρ<inf>B</inf> ∼1014.2 g/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 state and excited state properties of finite nuclei. We tabulate the outcome for various densities in terms of the pressure, free energy, entropy, etc. at a sufficiently large number of mesh points in the density range ρ<inf>B</inf> = 105.1 ∼1015.4 g/cm3, the temperature range <it>T</it>=0 ∼100 MeV and the proton fraction range <it>Y</it><inf>p</inf> = 0 ∼0.56 to be used for supernova simulations.

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