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.
Highlights
Another important dimension which makes the equation of state (EoS) of nuclear matter (NM) at finite temperature more interesting is the study of the dynamics of heavy ion collision reaction and 775 Page 2 of 14Eur
Many other important aspects of core-collapse events like how many protons are converted into neutrons, quenching rate, the mass-radius profile of newly born neutron star and its composition are determined by the EoS [8]. Another important dimension which makes the EoS of nuclear matter (NM) at finite temperature more interesting is the study of the dynamics of heavy ion collision reaction and
We start our discussion with the energy and pressure of hot NM and procurement of critical temperature for liquid-gas phase transition
Summary
Another important dimension which makes the EoS of nuclear matter (NM) at finite temperature more interesting is the study of the dynamics of heavy ion collision reaction and. Symmetry energy at finite temperature plays an important role in the cooling mechanism of newly born hot astrophysical objects [16,17,18] and has effective impact on the cooling rate through direct Urca and modified Urca processes [19,20]. We investigate the dependence of cooling mechanism of a hot dense matter on the EoS and the variation in the mass-radius profile of a proto-neutron star with temperature. The proton fraction in a newly born proto-neutron star depends on how the nuclear symmetry energy scales with density—which is an important aspect of this work [24]. The discussion and the concluding remarks are outlined in the Sect. 6
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