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Bayesian inference of neutron-skin thickness and neutron-star observables based on effective nuclear interactions
Nuclear Theory · Submitted 15 Apr 2024
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim While the neutron-skin thickness data (neutron-star observables) mostly constrain the symmetry energy at subsaturation (suprasaturation) densities, they may more or less constrain the behavior of the symmetry energy at suprasaturation (subsaturation) densities, depending on the energy-density functional form.
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The abstract, sentence by sentence
We have obtained the constraints on the density dependence of the symmetry energy from neutron-skin thickness data by parity-violating electron scatterings and neutron-star observables using a Bayesian approach, based on the standard Skyrme-Hartree-Fock (SHF) model and its extension as well as the relativistic mean-field (RMF) model. While the neutron-skin thickness data (neutron-star observables) mostly constrain the symmetry energy at subsaturation (suprasaturation) densities, they may more or less constrain the behavior of the symmetry energy at suprasaturation (subsaturation) densities, depending on the energy-density functional form. Besides showing the final posterior density dependence of the symmetry energy, we also compare the slope parameters of the symmetry energy at 0.10 fm$^{-3}$ as well as the values of the symmetry energy at twice saturation density from three effective nuclear interactions. The present work serves as a comparison study based on relativistic and non-relativistic energy-density functionals, for constraining the nuclear symmetry energy from low to high densities using a Bayesian approach.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We have obtained the constraints on the density dependence of the symmetry energy from neutron-skin thickness data by parity-violating electron scatterings and neutron-star observables using a Bayesian approach, based on the standard Skyrme-Hartree-Fock (SHF) model and its extension as well as the relativistic mean-field (RMF) model. | contribution 0.77 | 0.94 | 0.20 | asserted 1.00 |
| s1 | While the neutron-skin thickness data (neutron-star observables) mostly constrain the symmetry energy at subsaturation (suprasaturation) densities, they may more or less constrain the behavior of the symmetry energy at suprasaturation (subsaturation) densities, depending on the energy-density functional form. | interpretation 0.57 | 0.37 | 0.25 | hedged possibility 0.95 |
| s2 | Besides showing the final posterior density dependence of the symmetry energy, we also compare the slope parameters of the symmetry energy at 0.10 fm$^{-3}$ as well as the values of the symmetry energy at twice saturation density from three effective nuclear interactions. | contribution 0.69 | 0.92 | 0.14 | asserted 1.00 |
| s3 | The present work serves as a comparison study based on relativistic and non-relativistic energy-density functionals, for constraining the nuclear symmetry energy from low to high densities using a Bayesian approach. | contribution 0.97 | 0.72 | 0.14 | asserted 0.98 |
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The paper
Original abstract
We have obtained the constraints on the density dependence of the symmetry energy from neutron-skin thickness data by parity-violating electron scatterings and neutron-star observables using a Bayesian approach, based on the standard Skyrme-Hartree-Fock (SHF) model and its extension as well as the relativistic mean-field (RMF) model. While the neutron-skin thickness data (neutron-star observables) mostly constrain the symmetry energy at subsaturation (suprasaturation) densities, they may more or less constrain the behavior of the symmetry energy at suprasaturation (subsaturation) densities, depending on the energy-density functional form. Besides showing the final posterior density dependence of the symmetry energy, we also compare the slope parameters of the symmetry energy at 0.10 fm$^{-3}$ as well as the values of the symmetry energy at twice saturation density from three effective nuclear interactions. The present work serves as a comparison study based on relativistic and non-relativistic energy-density functionals, for constraining the nuclear symmetry energy from low to high densities using a Bayesian approach.
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What this paper does with the arXiv papers it cites
What it cites · 19 sentences without a confident label
Uses the method or tool of 2 papers
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The transition density between the liquid core and the inner crust is self-consistently determined from a thermodynamical approach as detailed in Refs. [ref] .
Nuclear constraints on properties of neutron star crusts · Theoretical framework · 0.93
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The EOS of the inner crust is parameterized based on an empirical polytropic relation between the pressure and the energy density [ref] .
Neutron Star Structure and the Equation of State · Theoretical framework · 0.86
Uses data or values from 8 papers
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We choose the neutron-skin thickness data $Δr_np = 0.283±0.071$ fm for $^208$Pb from PREX [ref] and $Δr_np= 0.121±0.035$ fm for $^48$Ca from CREX [ref] , so $d^exp_1,2$ and $σ_1,2$ in Eq. ([ref]) are chosen to be the mean values and $1σ$ errors, respectively.
Accurate Determination of the Neutron Skin Thickness of $^{208}$Pb through Parity-Violation in Electron Scattering · Theoretical framework · 1.00
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We choose the neutron-skin thickness data $Δr_np = 0.283±0.071$ fm for $^208$Pb from PREX [ref] and $Δr_np= 0.121±0.035$ fm for $^48$Ca from CREX [ref] , so $d^exp_1,2$ and $σ_1,2$ in Eq. ([ref]) are chosen to be the mean values and $1σ$ errors, respectively.
Precision Determination of the Neutral Weak Form Factor of $^{48}$Ca · Theoretical framework · 1.00
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In the present study, we construct the two-dimensional PDFs in the $M-R$ plane from the sampling data of the GW170817 event as well as the PSR J0030+0451 and the PSR J0740+6620, as those in Fig. 3 of Ref. [ref] , Fig. 20 of Ref. [ref] , and Fig. 7 of Ref. [ref] , respectively.
GW170817: Measurements of Neutron Star Radii and Equation of State · Theoretical framework · 0.88
Compares with 1 paper
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The posterior PDFs of symmetry energy parameters from both constraints of $Δr_np$ for $^48$Ca and $^208$Pb are compared with those from neutron-star observables [ref] in Fig. [ref].
Bayesian inference of neutron-star observables based on effective nuclear interactions · Results and discussions · 0.86
Cites as background 3 papers
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The nuclear symmetry energy $E_sym(ρ)$ is one of the most uncertain part of the nuclear matter equation of state (EOS), and great efforts have been devoted to extract its density dependence in the past twenty years [ref] .
Recent Progress and New Challenges in Isospin Physics with Heavy-Ion Reactions · Introduction · 0.99
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The nuclear symmetry energy $E_sym(ρ)$ is one of the most uncertain part of the nuclear matter equation of state (EOS), and great efforts have been devoted to extract its density dependence in the past twenty years [ref] .
Isospin Asymmetry in Nuclei and Neutron Stars · Introduction · 0.99
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The nuclear symmetry energy $E_sym(ρ)$ is one of the most uncertain part of the nuclear matter equation of state (EOS), and great efforts have been devoted to extract its density dependence in the past twenty years [ref] .
Neutron Star Observations: Prognosis for Equation of State Constraints · Introduction · 0.99
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