Microscopic Nuclear Equation of State with Three-Body Forces and Neutron Star Structure

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dc.creatorBaldo, M.
dc.creatorBurgio, G. F.
dc.creatorBombaci, I.
dc.date1996-07-10
dc.date.accessioned2026-07-07T05:41:43Z
dc.date.available2026-07-07T05:41:43Z
dc.descriptionWe 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 $M_{max} = 1.8 M_\odot$, a radius $R = 9.7$ km and a central density $n_c = 1.34~fm^{-3}$. We find the proton fraction exceeds the critical value $x^{Urca}$, for the onset of direct Urca processes, at densities $n \geq 0.45~fm^{-3}$. Therefore, in our model, NS's with masses above $M^{Urca} = 0.96 M_\odot$ 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.
dc.descriptionLaTeX, 10 pages, 4 Postscript figures included
dc.identifierhttps://arxiv.org/abs/nucl-th/9607013
dc.identifierhttp://arxiv.org/abs/nucl-th/9607013
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/82672
dc.subjectNuclear Theory
dc.subjectAstrophysics
dc.titleMicroscopic Nuclear Equation of State with Three-Body Forces and Neutron Star Structure
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