Systematic thermal reduction of neutronization in core-collapse supernovae

TL;DR

This study examines how temperature-dependent nuclear symmetry energy influences neutronization in core-collapse supernovae, revealing a small but consistent reduction in deleptonization that could impact shock wave energetics.

Contribution

It demonstrates that temperature dependence of symmetry energy causes a systematic, small reduction in neutronization during stellar collapse, with implications for supernova explosion modeling.

Findings

Small reduction (~0.4 foe) in shock dissociation energy due to symmetry energy effects.

Effect is robust across different electron capture strengths.

Supports further detailed supernova simulations.

Abstract

We investigate to what extent the temperature dependence of the nuclear symmetry energy can affect the neutronization of the stellar core prior to neutrino trapping during gravitational collapse. To this end, we implement a one-zone simulation to follow the collapse until beta equilibrium is reached and the lepton fraction remains constant. Since the strength of electron capture on the neutron-rich nuclei associated to the supernova scenario is still an open issue, we keep it as a free parameter. We find that the temperature dependence of the symmetry energy consistently yields a small reduction of deleptonization, which corresponds to a systematic effect on the shock wave energetics: the gain in dissociation energy of the shock has a small yet non-negligible value of about 0.4 foe (1 foe = 10^51 erg) and this result is almost independent from the strength of nuclear electron capture. The presence of such a systematic effect and its robustness under changes of the parameters of the one-zone model are significative enough to justify further investigations with detailed numerical simulations of supernova explosions.