arXiv:nucl-th/9802055·v1·Nuclear Theory
Neutron star properties with nuclear BHF equations of state
M. Baldo (INFN Sezione di Catania, Italy)🇮🇹 · G.F. Burgio (INFN Sezione di Catania, Italy)🇮🇹 · H.Q. Song (Academia Sinica, Shangai, China)🇨🇳 · F. Weber (University of Munich, Germany)🇩🇪
Abstract
We 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.
Comments: 8 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