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Hyperon stars in the Brueckner-Bethe-Goldstone theory
Nuclear Theory · Submitted 28 Dec 1999
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim This enhances enormously the hyperon population, and produces a strong softening of the equation of state, which turns out almost independent on the nucleon-nucleon interaction.
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The abstract, sentence by sentence
In the framework of the Brueckner-Bethe-Goldstone theory, we determine a fully microscopic equation of state for asymmetric and $\beta$-stable nuclear matter containing $\sim$ and $\la$ hyperons. We use the Paris and the new Argonne $Av_{18}$ two-body nucleon interaction, whereas the nucleon-hyperon interaction is described by the Njimegen soft-core model. We stress the role played by the three-body nucleon interaction, which produces a strong repulsion at high densities. This enhances enormously the hyperon population, and produces a strong softening of the equation of state, which turns out almost independent on the nucleon-nucleon interaction. We use the new equation of state in order to calculate the structure of static neutron stars. We obtain a maximum mass configuration with $M_{\rm max}$ = 1.26 (1.22) when the Paris ($Av_{18}$) nucleon potential is adopted. Central densities are about 10 times normal nuclear matter density. Stellar rotations, treated within a perturbative approach, increase the value of the limiting mass by about 12%.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | In the framework of the Brueckner-Bethe-Goldstone theory, we determine a fully microscopic equation of state for asymmetric and $\beta$-stable nuclear matter containing $\sim$ and $\la$ hyperons. | contribution 0.96 | 0.95 | 0.10 | asserted 1.00 |
| s1 | We use the Paris and the new Argonne $Av_{18}$ two-body nucleon interaction, whereas the nucleon-hyperon interaction is described by the Njimegen soft-core model. | method 1.00 | 0.57 | 0.03 | asserted 1.00 |
| s2 | We stress the role played by the three-body nucleon interaction, which produces a strong repulsion at high densities. | interpretation 0.39 | 0.53 | 0.12 | asserted 1.00 |
| s3 | This enhances enormously the hyperon population, and produces a strong softening of the equation of state, which turns out almost independent on the nucleon-nucleon interaction. | result 0.59 | 0.89 | 0.36 | asserted 1.00 |
| s4 | We use the new equation of state in order to calculate the structure of static neutron stars. | method 0.71 | 0.94 | 0.05 | asserted 0.94 |
| s5 | We obtain a maximum mass configuration with $M_{\rm max}$ = 1.26 (1.22) when the Paris ($Av_{18}$) nucleon potential is adopted. | result 1.00 | 0.96 | 0.37 | asserted 1.00 |
| s6 | Central densities are about 10 times normal nuclear matter density. | result 1.00 | 0.88 | 0.05 | asserted 1.00 |
| s7 | Stellar rotations, treated within a perturbative approach, increase the value of the limiting mass by about 12%. | result 1.00 | 0.92 | 0.11 | asserted 1.00 |
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Original abstract
In the framework of the Brueckner-Bethe-Goldstone theory, we determine a fully microscopic equation of state for asymmetric and $\beta$-stable nuclear matter containing $\sim$ and $\la$ hyperons. We use the Paris and the new Argonne $Av_{18}$ two-body nucleon interaction, whereas the nucleon-hyperon interaction is described by the Njimegen soft-core model. We stress the role played by the three-body nucleon interaction, which produces a strong repulsion at high densities. This enhances enormously the hyperon population, and produces a strong softening of the equation of state, which turns out almost independent on the nucleon-nucleon interaction. We use the new equation of state in order to calculate the structure of static neutron stars. We obtain a maximum mass configuration with $M_{\rm max}$ = 1.26 (1.22) when the Paris ($Av_{18}$) nucleon potential is adopted. Central densities are about 10 times normal nuclear matter density. Stellar rotations, treated within a perturbative approach, increase the value of the limiting mass by about 12%.
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References
How the literature uses it
12 arXiv papers cite this in 16 sentences
Papers citing it · 9 sentences without a confident label
Contests it 1 paper
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The complication here is that the non-relativistic theories we have thus far considered fail to account for the measured two-solar mass pulsars [ref] .
Superfluidity in nuclear systems and neutron stars · Hyperonic pairing · contest 0.88
Uses its method or tool 1 paper
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The EoS of hypernuclear matter is then constructed by using these interactions within the well known ab-initio microscopic Brueckner–Hartree–Fock (BHF) theory extended to the strange baryon sector [ref] .
Neutron Star Properties and Femtoscopic Constraints · Introduction · 0.95
Uses its data or values 1 paper
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Also Baldo et al. find values of $M_max = 1.26 M_⊙$ even when including three-body nucleon interactions [ref] .
Strangeness in Compact Stars · Masses of Neutron Stars · 0.86
Cites it as support 1 paper
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This implies that the EoS for strangeness-mixed matter is softer than neutron matter, as discussed in Refs. [ref] .
Properties of neutron stars and strangeness-mixed stars from a pion mean-field approach · Strageness-mixed stars · 0.96
Cites it as background 3 papers
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To consider the entire spin-1/2 baryon octet as part of the NS matter composition is almost the standard in the nuclear astrophysics community [ref] but, more recently, there is a strong interest in understanding how the presence of the $Δ$ baryons specifically may influence the properties of NS and their evolution [ref] .
Delta baryons in neutron stars · Introduction · 0.95
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However, asymmetric and $β$-stable nuclear matter could feature $Σ^-$ and $Λ$ hyperons [ref] .
Neutron Star Bounds on Muonic Fifth Forces from Picometer to Meter Scales · Introduction · 0.81
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The microscopic approaches are mainly based on lattice studies [ref] , many-particle theories employing the Brückner scattering matrix [ref] , Monte Carlo simulations [ref] and variational methods [ref] , see also the reviews [ref] .
Heavy Baryons in Compact Stars · Alternative approaches · 0.89
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