  Using the Boltzmann-radiation-hydrodynamics code, which solves the Boltzmann
equation for neutrino transport, we present the results of the simulations with
the nuclear equations of state (EOSs) of Lattimer and Swesty (LS) and Furusawa
and Shen (FS). We extend the simulation time of the LS model and conduct
thorough investigations, though our previous paper briefly reported some of the
results. Only the LS model shows the shock revival. This seems to originate
from the nuclear composition: the different nuclear composition results in the
different energy loss by photodissociation and hence the different strength of
the prompt convection and the later neutrino-driven convection. The
protoneutron star seen in the FS model is more compact than that in the LS
model because the existence of multinuclear species softens the EOS. For the
behavior of neutrinos, we examined the flux and the Eddington tensor of
neutrinos. In the optically thick region, the diffusion of neutrinos and the
dragging by the motion of matter determine the flux. In the optically thin
region, the free-streaming determines it. The Eddington tensor is compared with
that obtained from the M1-closure relation. The M1-closure scheme overestimates
the contribution from the velocity-dependent terms in the semitransparent
region.
