PUSHing core-collapse supernovae to explosions in spherical symmetry V: Equation of state dependency of explosion properties, nucleosynthesis yields, and compact remnants

TL;DR

This study uses the PUSH method to analyze how different nuclear equations of state influence supernova explosion properties, nucleosynthesis yields, and remnant types in spherical symmetry, across various progenitors and metallicities.

Contribution

It provides a comprehensive comparison of eight nuclear equations of state on supernova outcomes using a parametrized explosion model in spherical symmetry.

Findings

EOS-dependent differences in explosion energies and yields

No EOS can be ruled out based on current observational comparisons

Predicted remnant types vary with EOS and progenitor properties

Abstract

In this fifth paper of the series, we use the parametrized, spherically symmetric explosion method PUSH to investigate the impact of eight different nuclear equations of state (EOS). We present and discuss the explosion properties and the detailed nucleosynthesis yields, and predict the remnant (neutron star or black hole) for all our simulations. For this, we perform two sets of simulations. One, a complete study of non-rotating stars from 11 to 40 M$_{\odot}$ at three different metallicities using the SFHo EOS. And two, a suite of simulations for four progenitors (16 M$_{\odot}$ at three metallicities and 25 M$_{\odot}$ at solar metallicity) for eight different nuclear EOS. We compare our predicted explosion energies and yields to observed supernovae and to the metal-poor star HD~84937. We find EOS-dependent differences in the explosion properties and the nucleosynthesis yields. However, when comparing to observations, these differences are not large enough to rule out any EOS considered in this work.