Impact of the hot inner crust on compact stars at finite temperature

Abstract

We conducted a study on the thermal properties of stellar matter with the nuclear energy density functional BCPM. This functionalis based on microscopic Brueckner–Hartree–Fock calculations and has demonstrated success in describing cold neutron stars. Toenhance its applicability in astrophysics, we extended the BCPM equation of state to finite temperature for β-stable neutrino-freematter, taking into consideration the hot inner crust. Such an equation of state holds significant importance for hot compact objects,particularly those resulting from a binary neutron star merger event. Our exploration has shown that with increasing temperature,there is a fast decrease in the crust-core transition density, suggesting that for hot stars it is not realistic to assume a fixed value ofthis density. The microscopic calculations also reveal that the presence of nuclear clusters persists up to T = 7.21 MeV, identified asthe limiting temperature of the crust. Above this threshold, the manifestation of clusters is not anticipated. Below this temperature,clusters within the inner crust are surrounded by uniform matter with varying densities, allowing for the distinction between the upperand lower transition density branches. Moreover, we computed mass–radius relations of neutron stars, assuming an isothermal profilefor β-stable neutron star matter at various temperature values. Our findings highlight the significant influence of the hot inner crust onthe mass–radius relationship, leading to the formation of larger and more inflated neutron stars. Consequently, under our prescription,the final outcome is a unified equation of state at finite temperature.