Physics – Nuclear Physics
Scientific paper
Mar 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989nupha.493..549w&link_type=abstract
Nuclear Physics A, Volume 493, Issue 3-4, p. 549-582.
Physics
Nuclear Physics
35
Scientific paper
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 Msolar (MmaxH <= 2.44 Msolar when hyperons are taken into account). For the HF calculations we obtained MmaxHF <= 3.00 Msolar (MmaxHF <=2.85 Msolar). 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.
Weber Fridolin
Weigel Manfred K.
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