Neutron star properties with nuclear BHF equations of state

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dc.creatorBaldo, M.
dc.creatorBurgio, G. F.
dc.creatorSong, H. Q.
dc.creatorWeber, F.
dc.date1998-02-18
dc.date.accessioned2026-07-07T05:42:19Z
dc.date.available2026-07-07T05:42:19Z
dc.descriptionWe study the properties of static and rotating neutron stars adopting non-relativistic equations of state (EOS) for asymmetric nuclear matter based on the Brueckner-Hartree-Fock (BHF) scheme. The BHF calculation, with the continuous choice for the single particle potential, appears to be very close to the full EOS, which includes the three-hole line contribution calculated by solving the Bethe-Fadeev equations within the gap choice for the single particle potential. Three-body forces are included in order to reproduce the correct saturation point for nuclear matter. A comparison with fully relativistic many-body calculations of nuclear matter EOS is made.
dc.description8 pages, Latex, 3 figures included. To appear in "Hirschegg '98: Nuclear Astrophysics", Proceedings of Int. Workshop XXVI on Gross Properties of Nuclei and Nuclear Excitations, January 11-17 1998, Hirschegg, Austria
dc.identifierhttps://arxiv.org/abs/nucl-th/9802055
dc.identifierhttp://arxiv.org/abs/nucl-th/9802055
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/82885
dc.subjectNuclear Theory
dc.subjectAstrophysics
dc.titleNeutron star properties with nuclear BHF equations of state
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