Microscopic nuclear equation of state with threebody forces and neutron star structure
Abstract
We calculate static properties of nonrotating neutron stars (NS's) using a microscopic equation of state (EOS) for asymmetric nuclear matter, derived from the BruecknerBetheGoldstone manybody theory with explicit threebody forces. We use the Argonne AV14 and the Paris twobody nuclear force, implemented by the Urbana model for the threebody force. We obtain a maximum mass configuration with M_{max} = 1.8 M_☉ (M_{max} = 1.94 M_☉) 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 >= 0.65 fm(3) for the AV14 potential and n >= 0.54 fm(3) for the Paris potential. Therefore, NS's with masses above M(Urca) = 1.4 M_☉ for the AV14 and M(Urca) = 1.24 M_☉ 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.
 Publication:

Astronomy and Astrophysics
 Pub Date:
 December 1997
 arXiv:
 arXiv:astroph/9707277
 Bibcode:
 1997A&A...328..274B
 Keywords:

 DENSE MATTER;
 EQUATION OF STATE;
 STARS: NEUTRON;
 Astrophysics;
 Nuclear Theory
 EPrint:
 LaTeX, 10 pages, 7 figures included, accepted for publication in Astronomy &