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• W2078389739 abstract "A relativistic model of baryons interacting via the exchange of σ-, ω-, π- and ρ-mesons (scalar-vector-isovector (SVI) theory) is used to describe the properties of both dense and superdense matter. For the theoretical frame, we used the temperature-dependent Green's function formalism. The equation of state (EOS) is calculated for nuclear as well as neutron matter in the Hartree (H) and Hartree-Fock (HF) approximation. The existence of phase transitions has been investigated. The isotherms of pressure as a function of density show for nuclear matter a critical temperature of about TcHF = 16.6 MeV. (As in the usual scalar-vector (SV) theory, the phase transition is absent for neutron matter. A phase transition of both many-baryon systems in the high-pressure and high-density region, which has been found within the SV many-baryon theory, appears in the SVI theory too. The calculated maximum stable masses of neutron stars depend on (1) the underlying parameter set and/or (2) on the chosen approximation (i.e., H, HF; SV-, SVI theory, respectively). Hartree calculations lead to amass stability limit of MmaxH ⩽ 2.87 M⊙ (MmaxH ⩽ 2.44 M⊙ when hyperons are taken into account). For the HF calculations we obtained MmaxHF ⩽ 3.00 M⊙ (MmaxHF ⩽2.85 M⊙). The corresponding maximum radii are (same notation as above) RH ⩽ 13.2 km (RH ⩽ 11.8 km), RHF ⩽ 14.0 km (RHF 0 13.94km). The influence of the approximations, parameter sets and hyperons on the neutron star's moment of inertia is exhibited." @default.
• W2078389739 created "2016-06-24" @default.
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• W2078389739 date "1989-03-01" @default.
• W2078389739 modified "2023-10-16" @default.
• W2078389739 title "Neutron star properties and the relativistic nuclear equation of state of many-baryon matter" @default.
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• W2078389739 doi "https://doi.org/10.1016/0375-9474(89)90102-4" @default.
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