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.
From nuclear interactions to neutron star structure
BOMBACI, IGNAZIO;
1999-01-01
Abstract
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.File in questo prodotto:
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