Thermal impacts on the properties of nuclear matter and young neutron star

TL;DR

This paper investigates how temperature influences nuclear matter properties and proto-neutron star evolution using relativistic mean-field theory, providing insights into phase transitions, neutrino emission, and thermal stability.

Contribution

It introduces a temperature-dependent relativistic mean-field approach with new parameter sets to study nuclear matter and proto-neutron star properties, including phase transition and neutrino processes.

Findings

Critical temperature for liquid-gas phase transition matches experimental data.

Thermal index varies with nucleon density in relativistic and non-relativistic models.

Neutrino emissivity calculations reveal insights into proto-neutron star evolution.

Abstract

We present a methodical study of the thermal and nuclear properties for the hot nuclear matter using relativistic-mean field theory. We examine the effects of temperature on the binding energy, pressure, thermal index, symmetry energy, and its derivative for the symmetric nuclear matter using temperature-dependent relativistic mean-field formalism for the well-known G2$^{*}$ and recently developed IOPB-I parameter sets. The critical temperature for the liquid-gas phase transition in an asymmetric nuclear matter system has also been calculated and collated with the experimentally available data. We investigate the approach of the thermal index as a function of nucleon density in the wake of relativistic and non-relativistic formalism. The computation of neutrino emissivity through the direct Urca process for the supernovae remnants has also been performed, which manifests some exciting results about the thermal stabilization and evolution of the newly born proto-neutron star. The central temperature and the maximum mass of the proto-neutron star have also been calculated for different entropy values.