Systematic study of supernova equations of state at sub-nuclear densities with the Thomas-Fermi calculation

The nuclear equation of state (EOS) plays essential roles in numerical simulations of core-collapse supernovae, black hole formations, and binary neutron star mergers. Recently, we have constructed a new EOS table applicable to such simulations by using the cluster variational method for uniform matter and using the Thomas-Fermi calculation for non-uniform matter. In this study, it is found that the masses of heavy nuclides with our EOS are slightly larger than those with the Shen EOS in neutron-rich nuclear matter because of the smaller value of the density derivative coefficient of the symmetry energy in our EOS.

Motivated by this work, we investigate the dependence of the particle compositions in the low-density supernova matter on the empirical saturation values of the uniform EOS in more detail. For this purpose, we systematically construct the EOSs for non-uniform matter with the Thomas-Fermi calculation based on the macroscopic uniform EOS models.

In this presentation, we will report on the systematic properties of the non-uniform EOSs at finite temperature and discuss the effects of the saturation parameters included in the uniform EOS on the supernova matter in the low-density inhomogeneous region.