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An equation of state (EOS) for uniform nuclear matter is constructed at zero and finite temperatures with the variational method starting from the realistic nuclear Hamiltonian composed of the AV18 two-body potential and the UIX three-body potential. The maximum mass of the cold neutron star with this EOS is 2.2 M☉. Making use of uncertainty of the threebody nuclear force, adjustable parameters in the EOS are tuned so that the Thomas-Fermi calculations for β-stable nuclei reproduce the empirical data. The obtained EOS is appropriate for constructing a new nuclear EOS table for supernova simulations.

Nuclear Many-Body Approach for Supernova EOS: Thomas-Fermi Calculations of Non-Uniform Nuclear Matter