Numerical Study of Stellar Core Collapse and Neutrino Emission Using the Nuclear Equation of State Obtained by the Variational Method

TL;DR

This paper conducts numerical simulations of stellar core collapse using a nuclear equation of state derived from microscopic variational calculations, analyzing the impact on collapse dynamics, thermal structure, and neutrino emission across different progenitor masses.

Contribution

It introduces a new variational method-based nuclear EOS into core-collapse simulations and evaluates its effectiveness across various stellar progenitors.

Findings

The variational EOS performs well in all collapse scenarios.

Collapse dynamics and neutrino emission depend on the EOS used.

The study confirms the EOS's applicability to different stellar masses.

Abstract

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.