Bayesian analysis of the crust-core transition with a compressible liquid-drop model

Abstract

The crust-core phase transition of neutron stars is quantitatively studied within a unified meta-modelling of the nuclear Equation of State (EoS). The variational equations in the crust are solved within a Compressible Liquid Drop (CLD) approach, with surface parameters consistently optimized for each EoS set on experimental nuclear mass data. When EoS parameters are taken from known Skyrme or RMF functionals, the transition point of those models is nicely reproduced. A model-independent probability distribution of EoS parameters and of the transition density and pressure is determined with a Bayesian analysis, where the prior is given by an uncorrelated distribution of parameters within the present empirical uncertainties, and constraints are applied both from neutron star physics and ab-initio modelling. We show that the characteristics of the transition point are largely independent of the high density properties of the EoS, while ab-initio EoS calculations of neutron and symmetric matter are far more constraining. The most influential parameter for the determination of the transition point governs the surface properties of extremely neutron rich matter, and it is strongly unconstrained. This explains the large dispersion of existing predictions of the transition point. Only if the surface tension is fixed to a reasonable but somewhat arbitrary value, strong correlations with isovector parameters ($L_{sym},K_{sym}$ and $Q_{sym}$) are recovered. Within the present experimental and theoretical uncertainties on those parameters, we estimate the transition density as $n_t=0.072\pm 0.011$ fm${}^{-3}$ and the transition pressure as $P_t=0.339\pm 0.115$ MeV fm${}^{-3}$.

arXiv comment14 pages, 12 figures

References in corpus (67)

• A unified equation of state of dense matter and neutron star structure
• Equations of state for supernovae and compact stars
• Isospin Asymmetry in Nuclei and Neutron Stars
• Relativistic Equation of State of Nuclear Matter for Supernova and Neutron Star
• Neutron Star Structure and the Neutron Radius of 208Pb
• Constraints on the symmetry energy and neutron skins from experiments and theory
• The Equation of State of Hot, Dense Matter and Neutron Stars
• Further explorations of Skyrme-Hartree-Fock-Bogoliubov mass formulas. XII: Stiffness and stability of neutron-star matter
• Relativistic Mean-Field Hadronic Models under Nuclear Matter Constraints
• Constraining the Symmetry Parameters of the Nuclear Interaction
• Nuclear energy density optimization: Large deformations
• The Neutron Star Mass-Radius Relation and the Equation of State of Dense Matter
• Measuring the neutron star equation of state using X-ray timing
• Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
• Pulsar Constraints on Neutron Star Structure and Equation of State
• Neutron star radii and crusts: uncertainties and unified equations of state
• Error Estimates of Theoretical Models: a Guide
• A critical examination of constraints on the equation of state of dense matter obtained from GW170817
• Models of Pulsar Glitches
• Symmetry Energy II: Isobaric Analog States
• Low Mass Neutron Stars and the Equation of State of Dense Matter
• The equation of state for dense nucleonic matter from a metamodeling. I. Foundational aspects
• Surface Symmetry Energy
• Nuclear constraints on properties of neutron star crusts
• The Giant Dipole Resonance as a quantitative constraint on the symmetry energy
• Mapping crustal heating with the cooling lightcurves of quasi-persistent transients
• Core-crust transition in neutron stars: predictivity of density developments
• Inner crust of neutron stars with mass-fitted Skyrme functionals
• Density dependence of the nuclear symmetry energy: a microscopic perspective
• Neutron skin thickness in droplet model with surface width dependence: indications of softness of the nuclear symmetry energy
• Neutron star tidal deformabilities constrained by nuclear theory and experiment
• Asymmetric nuclear matter based on chiral two- and three-nucleon interactions
• The equation of state for dense nucleonic matter from a meta-modeling. II. Predictions for neutron stars properties
• Incompressibility of neutron-rich matter
• Using Neutron Star Observations to Determine Crust Thicknesses, Moments of Inertia, and Tidal Deformabilities
• Unified treatment of sub-saturation stellar matter at zero and finite temperature
• Unified equation of state for neutron stars on a microscopic basis
• Neutron star cooling after deep crustal heating in the X-ray transient KS 1731-260
• Equation of state and thickness of the inner crust of neutron stars
• Light nuclei quasiparticle energy shift in hot and dense nuclear matter
• Isospin-dependent clusterization of Neutron-Star Matter
• A survey of the parameter space of the compressible liquid drop model as applied to the neutron star inner crust
• Symmetry energy from the nuclear collective motion: constraints from dipole, quadrupole, monopole and spin-dipole resonances
• Surface Symmetry Energy of Nuclear Energy Density Functionals
• Origin of the neutron skin thickness of 208Pb in nuclear mean-field models
• Forecasting neutron star temperatures: predictability and variability
• Sensitivity of the Moment of Inertia of Neutron Stars to the Equation of State of Neutron-Rich Matter
• Nuclear matter fourth-order symmetry energy in the relativistic mean field models
• Magnetic neutron star cooling and microphysics
• Asymmetric semi-infinite nuclear matter: surface and curvature properties in relativistic and non-relativistic models
• Higher-order symmetry energy and neutron star core-crust transition with Gogny forces
• Nuclear matter equation of state including few-nucleon correlations $(A\le 4)$
• On the effect of high order empirical parameters on the nuclear equation of state
• Constraints on the symmetry energy from observational probes of the neutron star crust
• The decompression of the outer neutron star crust and r-process nucleosynthesis
• Constraints on the inner edge of neutron star crusts from relativistic nuclear energy density functionals
• Constraints on pulsar masses from the maximum observed glitch
• Model dependence of the neutron-skin thickness on the symmetry energy
• In-medium nuclear cluster energies within the Extended Thomas-Fermi approach
• Structures of the Vela pulsar and the glitch crisis from the Brueckner theory
• Cluster formation in asymmetric nuclear matter: semi-classical and quantal approaches
• Anomalous thermodynamics and phase transitions of neutron-star matter
• EoS constraints from nuclear masses and radii in a meta-modeling approach
• Correlation of the neutron star crust-core properties with the slope of the symmetry energy and the lead skin thickness
• Isospin-rich nuclei in neutron star matter
• Exact versus Taylor-expanded energy density in the study of the neutron star crust-core transition
• Estimating magnetar radii with an empirical meta-model

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• Science with the Einstein Telescope: a comparison of different designs
• Neutron Stars and the Nuclear Equation of State
• Dense Nuclear Matter Equation of State from Heavy-Ion Collisions
• The Science of the Einstein Telescope
• Uncertainties in the pasta-phase properties of catalysed neutron stars
• Curvature-slope correlation of nuclear symmetry energy and its imprints on the crust-core transition, radius and tidal deformability of canonical neutron stars
• Crystallization of the inner crust of a neutron star and the influence of shell effects
• Nucleonic metamodelling in light of multimessenger, PREX-II and CREX data
• Nuclear physics constraints from binary neutron star mergers in the Einstein Telescope era
• Investigating Dark Matter-Admixed Neutron Stars with NITR Equation of State in Light of PSR J0952-0607
• Constraining the nuclear symmetry energy and properties of neutron star from GW170817 by Bayesian analysis
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• Dense Matter in Neutron Stars with eXTP
• Prior probability distributions of neutron star crust models
• Bayesian inference of neutron-star observables based on effective nuclear interactions
• The effect of the energy functional on the pasta-phase properties of catalysed neutron stars
• A Bayesian analysis of the properties of hybrid stars with the NJL model
• Nuclear incompressibility and sound speed in uniform matter and finite nuclei
• Pasta properties of the neutron star within effective relativistic mean-field model
• Properties of the neutron star crust: Quantifying and correlating uncertainties with improved nuclear physics
• New quasi-universal relations for static and rapid rotating neutron stars
• Crustal properties of a neutron star within an effective relativistic mean-field model
• Confronting a set of Skyrme and ${\chi }_{EFT}$ predictions for the crust of neutron stars
• Detectability of a phase transition in neutron star matter with third-generation gravitational wave interferometers
• Comparison between the Thomas-Fermi and Hartree-Fock-Bogoliubov Methods in the Inner Crust of a Neutron Star: The Role of Pairing Correlations
• Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. IV. Role of the symmetry energy in pasta phases
• Empirical radius formulas for canonical neutron stars from bidirectionally selecting EOS features in extended Bayesian analyses of observational data
• From neutron skins and neutron matter to the neutron star crust
• Establishing connection between neutron star properties and nuclear matter parameters through a comprehensive multivariate analysis
• The proto-neutron star inner crust in the liquid phase
• Frozen and $\beta$-equilibrated $f$ and $p$ modes of cold neutron stars: nuclear metamodel predictions
• Crust-core interface and bulk neutron star properties
• Parametrization of the surface energy in the ETF approximation
• Statistical treatment of nuclear clusters in the continuum
• Ensembles of unified crust and core equations of state in a nuclear-multimessenger astrophysics environment
• Bayesian inference of neutron star crust properties using an ab initio-benchmarked meta-model
• Light clusters in the liquid proto-neutron star inner crust
• Crust (Unified) Tool for Equation-of-state Reconstruction (CUTER) v2
• Direct nonparametric multimessenger constraints on the equation of state of cold dense nuclear matter
• New Skyrme parametrizations to describe finite nuclei and neutron star matter with realistic effective masses
• Nuclear physics inputs for dense-matter modelling in neutron stars. The nuclear equation of state
• Effect of the equation of state for dilute neutron matter on the composition of the inner crust of neutron stars
• One- and two-argument equation of state parametrizations with continuous sound speed for neutron star simulations
• Statistical approach of nuclear multifragmentation with realistic nuclear equation of state
• Imprints of high-density nuclear symmetry energy on the crustal fraction of neutron star moment of inertia
• The nuclear matter density functional under the nucleonic hypothesis
• Neutron star crust properties: comparison between the compressible liquid-drop model and the extended Thomas-Fermi approach
• Tracing the Trace Anomaly of Dense Matter inside Neutron Stars
• Nuclear Drip Line and the Composition of Supernova Matter