Warm dense matter and cooling of supernovae remnants

TL;DR

This paper investigates how temperature influences nuclear matter properties and the cooling processes of supernova remnants, using relativistic mean-field models, and compares theoretical predictions with observational data.

Contribution

It provides a detailed analysis of thermal effects on nuclear matter properties and their implications for supernovae and neutron star observations using multiple relativistic models.

Findings

Critical temperature for liquid-gas phase transition aligns with previous studies.

Temperature effects on second differential coefficients show contrasting behaviors for different models.

G3 model's predictions support observations of massive pulsars and gravitational waves.

Abstract

We study the thermal effects on the nuclear matter (NM) properties such as binding energy, incompressibility, free symmetry energy and its coefficients using NL3, G3 and IU-FSU parameter sets of relativistic mean-field models. These models being consistent with the properties of cold NM, have also been used to study the effect of temperature by incorporating the Fermi function. The critical temperature for the liquid-gas phase transition in the symmetric NM is found to be 14.60, 15.37 and 14.50 MeV for NL3, G3 and IU-FSU parameter sets respectively, which is in excellent agreement with previous theoretical and experimental studies. We inspect that the properties related to second differential coefficient of the binding energy and free symmetry energy at saturation density ( i.e. K 0 (n, T ) and Q sym,0) exhibit the contrary effects for NL3 and G3 parameters as the temperature increases. We find that the prediction of saturated curvature parameter ( K sym,0 ) for G3 equation of state at finite temperature favour the combined analysis of K sym,0 for the existence of massive pulsars, gravitational waves from GW170817 and NICER observations of PSR J0030+0451. Further, we investigate the cooling mechanism of newly born stars through neutrino emissivity controlled by direct Urca process and instate some interesting remarks about neutrino emissivity. We also deliberate the effect of temperature on the M-R profile of Proto-Neutron star.