Microscopic nuclear equation of state with three-body forces and neutron star structure

We calculate static properties of non-rotating neutron stars (NS’s) using a microscopic equation of state (EOS) for asymmetric nuclear matter. The EOS is computed in the framework of the Brueckner–Bethe–Goldstone many–body theory. We introduce three-body forces in order to reproduce the correct saturation point of nuclear matter. A microscopic well behaved EOS is derived. We obtain a maximum mass configuration with Mmax = 1.8M⊙, a radius R = 9.7 km and a central density nc = 1.34 fm . We find the proton fraction exceeds the critical value x, for the onset of direct Urca processes, at densities n ≥ 0.45 fm. Therefore, in our model, NS’s with masses above M = 0.96M⊙ can undergo very rapid cooling depending on whether or not nucleon superfluidity in the interior of the NS takes place. A comparison with other microscopic models for the EOS is done, and neutron star structure is calculated for these models too. PACS numbers: 97.60.Jd, 21.65.+f