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