Effect of the Nuclear Equation of State on Relativistic-Turbulence Induced Core-Collapse Supernovae

TL;DR

This study investigates how different nuclear equations of state influence the success of core-collapse supernova explosions by analyzing their effects on turbulence and proto-neutron star properties in spherical models.

Contribution

It provides a systematic survey of various equations of state and links their impact on supernova viability to early entropy density and turbulence effects.

Findings

Explosion viability depends on the EOS and correlates with early interior entropy density.

Higher central entropies lead to more vigorous proto-neutron-star convection.

Progenitor mass has limited effect on the EOS influence, except for low-mass stars.

Abstract

The nuclear equation of state is an important component in the evolution of core collapse supernovae. In this paper we make a survey of various equations of state in the literature and analyze their effect on spherical core-collapse models in which the effects of three-dimensional turbulence is modeled by a general relativistic formulation of Supernova Turbulence in Reduced dimensionality (STIR). We show that the viability of the explosion is quite EOS dependent and that it best correlates with the early-time interior entropy density of the proto-neutron star. We check that this result is not progenitor dependent, although low-mass progenitors show different explosion properties, due to the different pre-collapse nuclear composition. Larger central entropies also induce more vigorous proto-neutron-star convection in our one-dimensional turbulence model, as well as a wider convective layer.