Hyperonic equation of state at finite temperature for neutron stars

TL;DR

This paper reviews the hyperonic core composition and equation of state of neutron stars at finite temperature using an improved relativistic mean-field model, highlighting the impact of hyperons on neutron star properties.

Contribution

It introduces an extended FSU2H* model incorporating recent Xi potential data and finite temperature effects for detailed neutron star core analysis.

Findings

Hyperons significantly alter the composition at finite temperature.

The equation of state is strongly affected by hyperonic inclusion.

Results are relevant for understanding hot neutron star evolution.

Abstract

We review the composition and the equation of state of the hyperonic core of neutron stars at finite temperature within a relativistic mean-field approach. We make use of the new FSU2H* model, which is built upon the FSU2H scheme by improving on the Xi potential according to the recent analysis on the Xi atoms, and we extend it to include finite temperature corrections. The calculations are done for a wide range of densities, temperatures and charge fractions, thus exploring the different conditions that can be found in protoneutron stars, binary mergers remnants and supernovae explosions. The inclusion of hyperons has a strong effect on the composition and the equation of state at finite temperature, which consequently would lead to significant changes in the properties and evolution of hot neutron stars.