New Table of Supernova Equation of State Using a Variational Method and Its Application to Astrophysical Compact Objects

Abstract

We have constructed a new equation of state (EOS) for dense nuclear matter based on a variational many-body theory. For the homogeneous phase, the free energy is calculated by the cluster variational method with the realistic nuclear Hamiltonian composed of the Argonne v18 two-nucleon and Urbana IX three-nucleon potentials. For the inhomogeneous phase, the Thomas-Fermi approximation is adopted so as to construct the EOS of non-uniform matter which is consistent with that of uniform phase. It is found that the obtained EOS shows the higher critical temperature and larger mass numbers of nuclides in neutron-rich nuclear matter, as compared with the Shen EOS. We tabulate the present EOS in wade ranges of the temperature, proton fraction, and baryon density. Using the resultant EOS table, we finally perform the calculation of protoneutron star structures and the simple supernova simulation to investigate the properties of our EOS.