2026-07-072026-07-07http://salesiana.dossiersoluciones.com/handle/123456789/82885We 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.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, AustriaNuclear TheoryAstrophysicstext