Microscopic nuclear equation of state at finite temperature and stellar stability

TL;DR

This paper develops a microscopic nuclear equation of state compatible with astrophysical data, extends it to finite temperature, and investigates its impact on neutron star properties and stability.

Contribution

It introduces a consistent finite-temperature extension of a microscopic nuclear equation of state within the Brueckner-Hartree-Fock framework, analyzing neutron star stability.

Findings

Finite temperature affects neutron star properties significantly.

A universal relation for stellar stability is proposed.

The equation of state aligns with current astrophysical constraints.

Abstract

A microscopic nuclear equation of state compatible with all current astrophysical constraints constructed within the Brueckner-Hartree-Fock formalism is presented and extended in a consistent way to finite temperature. The effects of finite temperature on the properties of neutron stars are studied in detail and a universal relation regarding stellar stability is proposed.