Light nuclei in supernova envelopes: a quasiparticle gas model

TL;DR

This paper develops an equation of state for low-density supernova matter containing light nuclei using a quasiparticle gas model, highlighting the role of clusters and their impact on critical temperature for deuteron condensation.

Contribution

It introduces a quasiparticle gas model incorporating bound states and Skyrme functional to describe supernova matter with light nuclei, providing new insights into cluster formation and phase transitions.

Findings

Deuterons, tritons, and 3H(e) nuclei have higher concentrations than heavier nuclei.

The presence of clusters lowers the critical temperature for deuteron condensation.

The model accounts for bound states with decay times relevant to supernova evolution.

Abstract

We present an equation of state and the composition of low-density supernova matter composed of light nuclei with mass number A \le 13. We work within the quasiparticle gas model, which accounts for bound states with decay time scales larger than the relevant time scale of supernova and protoneutron star evolution. The mean-field contribution is included in terms of Skyrme density functional. Deuterons, tritons, and 3H(e) nuclei appear in matter in concentrations that are substantially higher than those of heavier nuclei. We calculate the critical temperature of deuteron condensation in such matter, and demonstrate that the appearance of clusters substantially lowers the critical temperature.