dorsal/arxiv
View SchemaMicroscopic Nuclear Equation of State with Three-Body Forces and Neutron Star Structure
| Authors | M. Baldo, G. F. Burgio, I. Bombaci |
|---|---|
| Categories | |
| ArXiv ID | nucl-th/9607013 |
| URL | https://arxiv.org/abs/nucl-th/9607013 |
Abstract
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 $M_{max} = 1.8 M_\odot$, 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.
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"abstract": "We calculate static properties of non-rotating neutron stars (NS\u0027s) using a\nmicroscopic equation of state (EOS) for asymmetric nuclear matter. The EOS is\ncomputed in the framework of the Brueckner--Bethe--Goldstone many--body theory.\nWe introduce three-body forces in order to reproduce the correct saturation\npoint of nuclear matter. A microscopic well behaved EOS is derived. We obtain a\nmaximum mass configuration with $M_{max} = 1.8 M_\\odot$, a radius $R = 9.7$ km\nand a central density $n_c = 1.34~fm^{-3}$. We find the proton fraction exceeds\nthe critical value $x^{Urca}$, for the onset of direct Urca processes, at\ndensities $n \\geq 0.45~fm^{-3}$. Therefore, in our model, NS\u0027s with masses\nabove $M^{Urca} = 0.96 M_\\odot$ can undergo very rapid cooling depending on\nwhether or not nucleon superfluidity in the interior of the NS takes place. A\ncomparison with other microscopic models for the EOS is done, and neutron star\nstructure is calculated for these models too.",
"arxiv_id": "nucl-th/9607013",
"authors": [
"M. Baldo",
"G. F. Burgio",
"I. Bombaci"
],
"categories": [
"nucl-th",
"astro-ph"
],
"title": "Microscopic Nuclear Equation of State with Three-Body Forces and Neutron Star Structure",
"url": "https://arxiv.org/abs/nucl-th/9607013"
},
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