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Using the Boltzmann-radiation-hydrodynamics code, which solves the Boltzmannequation for neutrino transport, we present the results of the simulations withthe nuclear equations of state (EOSs) of Lattimer and Swesty (LS) and Furusawaand Shen (FS). We extend the simulation time of the LS model and conductthorough investigations, though our previous paper briefly reported some of theresults. Only the LS model shows the shock revival. This seems to originatefrom the nuclear composition: the different nuclear composition results in thedifferent energy loss by photodissociation and hence the different strength ofthe prompt convection and the later neutrino-driven convection. Theprotoneutron star seen in the FS model is more compact than that in the LSmodel because the existence of multinuclear species softens the EOS. For thebehavior of neutrinos, we examined the flux and the Eddington tensor ofneutrinos. In the optically thick region, the diffusion of neutrinos and thedragging by the motion of matter determine the flux. In the optically thinregion, the free-streaming determines it. The Eddington tensor is compared withthat obtained from the M1-closure relation. The M1-closure scheme overestimatesthe contribution from the velocity-dependent terms in the semitransparentregion.

the astrophysical journal

The Boltzmann-radiation-hydrodynamics Simulations of Core-collapse  Supernovae with Different Equations of State: the Role of Nuclear Composition  and the Behavior of Neutrinos