Impact of the nuclear equation of state on the explodability of massive stars

TL;DR

This study uses multi-dimensional simulations to explore how different nuclear equations of state influence the likelihood of massive star explosions, highlighting the significant uncertainty and the need for better nuclear physics constraints.

Contribution

It demonstrates the impact of various nuclear equations of state on supernova explodability using 2D simulations, emphasizing the importance of nuclear physics in astrophysical outcomes.

Findings

Explosions occur more frequently with SFHo and SFHx EoS.

CMF EoS leads to fewer explosions, only in 2 out of 15 cases.

Lower neutrino luminosities and weaker proto-neutron star contraction reduce explodability with CMF.

Abstract

In recent years, astrophysical observations have placed tight constraints on key properties of the nuclear equation of state (EoS). Using 45 two-dimensional simulations for three different EoS compatible with the current tight constraints, we show that the EoS remains a major uncertainty for the outcome of core-collapse supernovae. Whereas explosions are obtained in most cases for the SFHo and SFHx EoS, for the CMF EoS, which includes a crossover from nucleonic matter to a quark phase, explosions occur only for 2 out of 15 progenitors. Less favourable conditions for neutrino-driven explosions arise for the CMF EoS due to lower neutrino luminosities and mean energies and slightly weaker contraction of the warm proto-neutron star. Our results suggest that the explodability of massive stars cannot yet be predicted based on first principles without better knowledge of the nuclear EoS. Conversely, observational constraints on stellar explodability may help further constrain the EoS.