Particular Properties of Dense Supernova Matter : Nuclear Physics

概要

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Dense supernova matter composed of n, p, e^-, e^+, ν_e and ν^^-_e is investigated in detail by solving self-consistently a set of finite-temperature Hartree-Fock equations with an effective nucleon interaction. The effective interaction includes a phenomenological three-nucleon interaction to assure the saturation property of symmetric nuclear matter. Results of thermodynamic quantities and mixing ratios of respective components are analyzed and tabulated for wide region of density (ρ=(1-6)ρ_ο) and temperature (T=(10-40) MeV) by choosing the lepton fraction Y_l=(0.3, 0.35, 0.4). We discuss particular properties of the matter such as the constancy of composition, the large proton fraction expressed by Y_p≃(2/3)Y_l+0.05 and the stiffened equation of state, and also discuss remarkable features of hot neutron stars at birth such as the fat density profile and the increasing temperature toward the center. It is shown that these features are caused essentially by the effects of neutrino trapping to generate the high and constant lepton fraction and isentropic nature, the effects which are absent in neutron star matter.
理論物理学刊行会の論文
1994-10-25