Numerical study of stellar core collapse and neutrino emission using the nuclear equation of state obtained by the variational method

Core-collapse simulations of massive stars are performed using the equation of state (EOS) based on the microscopic variational calculation with realistic nuclear forces. Progenitor models with initial masses of 15, 9.6, and 30 M· are adopted as examples of an ordinary core-collapse supernova with a shock stall, a low-mass supernova with a successful explosion, and black hole formation, respectively. Moreover, the neutrinos emitted from the stellar collapse are assessed. The variational EOS is confirmed to work well in all cases. The EOS dependencies of the dynamics, thermal structure, and neutrino emission of the stellar collapse are also investigated.