Thermal effects on the baryon-quark phase transition in hot hybrid neutron stars: a statistical mean-field baryonic model with the standard NJL model for deconfined quarks

We investigate the thermal effects on the baryon-quark phase transition (PT), utilizing the Maxwell construction (MC) in an isentropic analysis. In order to model the structure and composition of hot hybrid neutron stars (HHNSs) with beta-equilibrated dense matter in the presence (absence) of trapped neutrinos, we use a statistical model which agrees with the Thomas-Fermi (TF) approximation for the baryonic phase and the Nambu-Jona-Lasinio (NJL) model for the deconfined quark phase. Our results show that neutrino trapping can provide a considerable softening of the equation of state EOS in the baryon-quark coexistence phase, compared with the situation governed by untrapped (free-streaming) neutrinos. Having a weak dependence on the quark vector coupling constant in the pure quark phase, the temperature meets its maximum value at the threshold baryonic density for the occurrence of the baryon-quark PT. Based on the assumption of the conserved baryonic mass, all of our HHEOS lead to the stable mass structures for a HHNS.