Bayesian inference of neutron-skin thickness and neutron-star observables based on effective nuclear interactions

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.

arXiv comment10 pages, 7 figures

References in corpus (40)

• GW170817: Measurements of Neutron Star Radii and Equation of State
• A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation
• Neutron Star Structure and the Equation of State
• Neutron Star Observations: Prognosis for Equation of State Constraints
• Recent Progress and New Challenges in Isospin Physics with Heavy-Ion Reactions
• A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy
• Equations of state for supernovae and compact stars
• Isospin Asymmetry in Nuclei and Neutron Stars
• Accurate Determination of the Neutron Skin Thickness of ${}^{208}$Pb through Parity-Violation in Electron Scattering
• Pulsar Constraints on Neutron Star Structure and Equation of State
• Constraining the neutron-proton effective mass splitting using empirical constraints on the density dependence of nuclear symmetry energy around normal density
• Constraining Neutron-Star Matter with Microscopic and Macroscopic Collisions
• Nuclear Matter and its Role in Supernovae, Neutron Stars and Compact Object Binary Mergers
• Precision Determination of the Neutral Weak Form Factor of ${}^{48}$Ca
• Density slope of the nuclear symmetry energy from the neutron skin thickness of heavy nuclei
• Symmetry Parameter Constraints From A Lower Bound On The Neutron-Matter Energy
• Building relativistic mean field models for finite nuclei and neutron stars
• The equation of state for dense nucleonic matter from a metamodeling. I. Foundational aspects
• The Compression-Mode Giant Resonances and Nuclear Incompressibility
• Nuclear constraints on properties of neutron star crusts
• Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817
• Constraining the symmetry energy at subsaturation densities using isotope binding energy difference and neutron skin thickness
• Constraining the nuclear equation of state at subsaturation densities
• Symmetry energy from the nuclear collective motion: constraints from dipole, quadrupole, monopole and spin-dipole resonances
• Locating the inner edge of neutron star crust using terrestrial nuclear laboratory data
• Bayesian Inference of the Symmetry Energy of Super-Dense Neutron-Rich Matter from Future Radius Measurements of Massive Neutron Stars
• Constraints on the symmetry energy and its associated parameters from nuclei to neutron stars
• Decoding the Density Dependence of the Nuclear Symmetry Energy
• Spin-Down of Neutron Stars and Compositional Transitions in the Cold Crustal Matter
• How tightly is nuclear symmetry energy constrained by unitary Fermi gas?
• Phase Transition Study meets Machine Learning
• Bayesian inference of nuclear symmetry energy from measured and imagined neutron skin thickness in ${}^{116,118,120,122,124,130,132}$Sn, ${}^{208}$Pb, and ${}^{48}$Ca
• Prediction of Nuclear Charge Density Distribution with Feedback Neural Network
• Constraining the density dependence of the symmetry energy with nuclear data and astronomical observations in the KIDS framework
• Bayesian refinement of covariant energy density functionals
• Bayesian inference of neutron-star observables based on effective nuclear interactions
• Constraining three-nucleon forces with multimessenger data
• Relativistic approach for the determination of nuclear and neutron star properties in consideration of PREX-II results
• Equation of state of nuclear matter and neutron stars: Quark mean-field model versus relativistic mean-field model
• Bayesian inference of finite-nuclei observables based on the KIDS model

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