Effects of nuclear matter and composition in core-collapse supernovae and long-term proto-neutron star cooling

TL;DR

This paper investigates how different nuclear equations of state and compositional treatments influence core-collapse supernova dynamics and proto-neutron star cooling, revealing significant impacts on collapse, shock propagation, and neutrino emission.

Contribution

It compares microscopic nuclear EOS models and compositional treatments, highlighting their effects on supernova simulations and proto-neutron star evolution.

Findings

Different EOS models significantly affect collapse and shock dynamics.

Compositional differences impact proto-neutron star cooling and neutrino emission.

Modeling choices in nuclear matter and composition are crucial for accurate supernova simulations.

Abstract

We study the influence of hot and dense matter in core-collapse supernovae by adopting up-to-date nuclear equation of state (EOS) based on the microscopic nuclear many-body frameworks. We explore effects of EOS based on the Dirac Brueckner Hartree-Fock theory through comparisons with those based on the variational method. We also examine effects of the differences in the composition of nuclei and nucleons by using the same EOS by the variational method but employing two different treatments in computations of nuclear abundances. We perform numerical simulations of core-collapse supernovae adopting the three EOSs. We also perform numerical simulations of the long-term evolution over 70 s of the proto-neutron star cooling. We show that impacts by different modeling of composition are remarkable as in those by different treatments of uniform matter in the gravitational collapse, bounce, and shock propagation. The cooling of proto-neutron star and the resulting neutrino emission are also affected by the compositional difference even if the same treatment in computing uniform matter of EOS.