Proto-neutron stars in the Thomas-Fermi theory

چکیده مقاله

The structure and composition of proto-neutron stars (PNSs) are studied by the equation of state (EOS) of hot baryonic matter in β−equilibrium. On the basis of the Landau Fermi-liquid theory (LFT), the Thomas-Fermi (TF) approximation is used in a semi-classical mean-field (MF) model to present an isentropic description of PNS matter including hyperons. Our findings for the PNS structure indicate that higher values of the proton abundance may exist at higher baryonic densities. In addition, the maximum mass of PNSs is increased by the effects of neutrino trapping and, therefore, rising of the lepton number, since the EOS of PNS matter becomes stiffer. However, this maximum value is slightly affected by the changes in the entropy per baryon.