Hartree-Fock Formulation of the QMC Model at Finite Temperature

TL;DR

This paper develops a detailed relativistic mean field model including Fock terms for high-density, finite-temperature matter with the full baryon octet, relevant for neutron star and merger simulations.

Contribution

It introduces a comprehensive finite-temperature QMC model with Fock terms, extending previous zero-temperature models for astrophysical applications.

Findings

Fock terms significantly affect the energy density functional.

The model accurately describes proto-neutron star properties.

Results align with observational data on neutron stars.

Abstract

We present, for the first time, a detailed theory of high density matter including the entire baryon octet at finite temperature, based on a fully relativistic mean field model with a consistent treatment of exchange (Fock) terms, using the quark-meson-coupling model (QMC). It has been already demonstrated that the QMC equation of state is applicable in thermodynamic scenarios in stationary and rotating isentropic proto-neutron stars, producing results in agreement with recent observation. It is also suitable for the simulation of the behavior following a binary neutron star merger [1]; https://compose.obspm.fr/eos/205. We develop a comprehensive demonstration of the impact of the Fock terms in the QMC energy density functional on properties of neutrinoless proto-neutron stars with cores containing the full hyperon octet with constant entropy, S/A=2kB. Given the interest in the properties of the proto-neutron star remaining after either a supernova explosion or the merger of two neutron stars, it is vital to develop modern equations of state at finite temperature. While much attention has been paid to relativistic mean-field calculations at finite temperature, it is crucial to explore the consequences of a consistent treatment of the Fock terms.