Bayesian analysis of astrophysical and laboratory data favors the two-families scenario of coexisting hadronic and strange quark stars over the one-family scenario.
Do hyperons exist in the interior of neutron stars ?
6 Pith papers cite this work. Polarity classification is still indexing.
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abstract
In this work we review the role of hyperons on the properties of neutron and proto-neutron stars. In particular, we revise the so-called "hyperon puzzle", go over some of the solutions proposed to tackle it, and discuss the implications that the recent measurements of unusually high neutron star masses have on our present knowledge of hypernuclear physics. We reexamine also the role of hyperons on the cooling properties of newly born neutron stars and on the so-called r-mode instability.
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White dwarf mass-radius data exclude large parameter space for ultralight scalars quadratically coupled to fermions by predicting forbidden radius gaps and mass shifts toward the Chandrasekhar limit or altered maximum masses.
Hybrid neutron-star equations of state remain sensitive to the low-density nucleonic model at transition densities around 2ρ₀, with model spread in radius and tidal deformability exceeding observational uncertainty by factors of ~1.8 and ~1.4.
Including hyperons reduces maximum neutron-star mass by 0.05-0.10 solar masses and increases radius at 1.4 solar masses by 0.5-0.8 km across all models while keeping every equation of state consistent with the 2-solar-mass limit.
Systematic scan of ΛNN and ΛΛN three-body force parameters in Skyrme EDF for beta-equilibrated hyperonic matter, TOV branch classification, and Bayesian analysis with XGBoost-SHAP on NS mass-radius constraints.
Adding Pomeron exchange to the NΩ system improves agreement with experiment in the ^5S2 channel and predicts a weak quasi-bound state in the ^3S1 channel.
citing papers explorer
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Is the coexistence of strange quark stars and hadronic stars favored by astrophysical data? A Bayesian analysis
Bayesian analysis of astrophysical and laboratory data favors the two-families scenario of coexisting hadronic and strange quark stars over the one-family scenario.
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$\phi$-Dwarfs: White Dwarfs probe Quadratically Coupled Scalars
White dwarf mass-radius data exclude large parameter space for ultralight scalars quadratically coupled to fermions by predicting forbidden radius gaps and mass shifts toward the Chandrasekhar limit or altered maximum masses.
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Sensitivity of Neutron Star Observables to Transition Density in Hybrid Equation-of-State Models
Hybrid neutron-star equations of state remain sensitive to the low-density nucleonic model at transition densities around 2ρ₀, with model spread in radius and tidal deformability exceeding observational uncertainty by factors of ~1.8 and ~1.4.
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Hyperonic equation of state for neutron stars: A systematic Bayesian comparison of density-dependent and non-linear relativistic mean-field models
Including hyperons reduces maximum neutron-star mass by 0.05-0.10 solar masses and increases radius at 1.4 solar masses by 0.5-0.8 km across all models while keeping every equation of state consistent with the 2-solar-mass limit.
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Impact of hyperon mixing on neutron star structure based on Skyrme-type equations of state: Systematic analysis of $\Lambda NN$ and $\Lambda\Lambda N$ three-body forces with Bayesisan inference
Systematic scan of ΛNN and ΛΛN three-body force parameters in Skyrme EDF for beta-equilibrated hyperonic matter, TOV branch classification, and Bayesian analysis with XGBoost-SHAP on NS mass-radius constraints.
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Near-threshold scattering of proton and Omega baryon and possible bound states
Adding Pomeron exchange to the NΩ system improves agreement with experiment in the ^5S2 channel and predicts a weak quasi-bound state in the ^3S1 channel.