MICROSCOPIC NUCLEAR-EQUATION OF STATE WITH 3-BODY FORCES AND NEUTRON-STAR STRUCTURE

We calculate static properties of non-rotating neutron stars INS's) us ing a microscopic equation of state (EOS) for asymmetric nuclear matte r, derived from the Brueckner-Bethe-Goldstone many-body theory with ex plicit three-body forces. We use the Argonne AV 14 and the Paris two-b ody nuclear force, implemented by the Urbana model for the three-body force, We obtain a maximum mass configuration with M-max = 1.8M. (M-ma x = 1.94M.) when the AV14 (Paris) interaction is used. They are both c onsistent with the observed range of NS masses. The onset of direct Ur ea processes occurs al densities n greater than or equal to 0.65 fm(-3 ) for the AV14 potential and n greater than or equal to 0.54 fm(-3) fo r the Paris potential. Therefore, NS's with masses above M-Urca = 1.4M . for the AV14 and M-Urca = 1.24M. for the Paris potential can undergo very rapid cooling, depending on the strength of superfluidity in the interior of the NS. The comparison with other microscopic models for the EOS shows noticeable differences.