We calculate static properties of non-rotating neutron stars ( NS ’ s ) using a microscopic equation of state ( EOS ) for asymmetric nuclear matter , derived from the Brueckner–Bethe–Goldstone many–body theory with explicit three-body forces .
We use the Argonne AV14 and the Paris two–body nuclear force , implemented by the Urbana model for the three-body force .
We obtain a maximum mass configuration with M _ { max } = 1.8 M _ { \sun } ( M _ { max } = 1.94 M _ { \sun } ) when the AV14 ( Paris ) interaction is used .
They are both consistent with the observed range of NS masses .
The onset of direct Urca processes occurs at densities n \geq 0.65 ~ { } fm ^ { -3 } for the AV14 potential and n \geq 0.54 ~ { } fm ^ { -3 } for the Paris potential .
Therefore , NS ’ s with masses above M ^ { Urca } = 1.4 M _ { \sun } for the AV14 and M ^ { Urca } = 1.24 M _ { \sun } 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 .