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Microscopic nuclear equation of state with three-body forces and neutron star structure
Astrophysics · Submitted 25 Jul 1997
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim 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.
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The abstract, sentence by sentence
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.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | 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. | contribution 0.82 | 0.96 | 0.10 | asserted 1.00 |
| s1 | We use the Argonne AV14 and the Paris two-body nuclear force, implemented by the Urbana model for the three-body force. | method 1.00 | 0.57 | 0.02 | asserted 1.00 |
| s2 | 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. | result 1.00 | 0.95 | 0.33 | asserted 1.00 |
| s3 | They are both consistent with the observed range of NS masses. | interpretation 0.89 | 0.53 | 0.14 | asserted 0.65 |
| s4 | 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. | result 1.00 | 0.92 | 0.07 | asserted 1.00 |
| s5 | 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. | interpretation 0.73 | 0.87 | 0.22 | hedged possibility 0.73 |
| s6 | The comparison with other microscopic models for the EOS shows noticeable differences. | result 0.77 | 0.65 | 0.06 | asserted 1.00 |
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The paper
Original 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. 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.
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References
How the literature uses it
10 arXiv papers cite this in 13 sentences
Papers citing it · 9 sentences without a confident label
Uses its method or tool 1 paper
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We consider in this work two microscopic EOSs that have been derived within the BHF formalism [ref] based on realistic two-nucleon ($NN$) and compatible three-nucleon forces (TBF) [ref] , namely those employing the Argonne $V_18$ [ref]
Accurate nuclear symmetry energy at finite temperature within a BHF approach · Introduction · 0.89
Uses its data or values 1 paper
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Name Particle Calculation Method Inhomogeneous Reference Content Homogeneous Matter Matter APR(APR) npe$μ$ Microscopic calculations Crust-core matched [ref] BBB(BHF-BBB2) npe Microscopic calculations Crust-core matched [ref] BL(chiral) npe$μ$N Microscopic calculations Unified EoS [ref] BSK20 2*npe$μ$ 2*Non-relativ. density functional 2*Unified EoS 2* [ref] BSK21 PCP(BSK22) npe$μ$N Non-relativ. density functional Unified EoS 4* [ref] PCP(BSK24) npe$μ$N Non-relativ. density functional Unified EoS PCP(BSK25) npe$μ$N Non-relativ. density functional Unified EoS PCP(BSK26) npe$μ$N Non-relativ. density functional Unified EoS ENG npe Non-relativ. density functional Crust-core matched [ref] KDE0v npe$μ$ Non-relativ. density functional Unified EoS 2* [ref] KDE0v1 npe$μ$ Non-relativ. density functional Unified EoS MPA1 npe Relativistic density functional Not treated [ref] RS npe$μ$ Non-relativ. den
Direct nonparametric multimessenger constraints on the equation of state of cold dense nuclear matter · Equation of state training catalog · 0.95
Compares with it 1 paper
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This is a different approach with respect to other well known microscopic EOS models for $β$-stable nuclear matter, as e.g. the APR [ref] EOS or the BBB [ref] EOS.
Effects of Chiral Effective Field Theory Equation of State on Binary Neutron Star Mergers · The BL Equation of State · 0.91
Cites it as background 1 paper
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In the literature, two standard approaches have been used: ab-initio calculations, see e.g. Refs. [ref] , and phenomenological models, see e.g. Refs. [ref] , both having their advantages and drawbacks.
Relativistic mean-field predictions for dense matter equation of state and application to neutron stars · Introduction · 1.00
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