Correlation of the neutron star crust-core properties with the slope of the symmetry energy and the lead skin thickness

Abstract

The correlations of the crust-core transition density and pressure in neutron stars with the slope of the symmetry energy and the neutron skin thickness are investigated, using different families of relativistic mean field parametrizations with constant couplings and non-linear terms mixing the $\sigma$, $\omega$ and $\rho$-meson fields. It is shown that the modification of the density dependence of the symmetry energy, involving the $\sigma$ or the $\omega$ meson, gives rise to different behaviors: the effect of the $\omega$-meson may also be reproduced within non-relativistic phenomenological models, while the effect of the $\sigma$-meson is essentially relativistic. Depending on the parametrization with $\sigma -\rho$ or $\omega -\rho$ mixing terms, different values of the slope of the symmetry energy at saturation must be considered in order to obtain a neutron matter equation of state compatible with results from chiral effective field theory. This difference leads to different pressures at the crust-core transition density. A linear correlation between the transition density and the symmetry energy slope or the neutron skin thickness of the ${}^{208}$Pb nucleus is obtained, only when the $\omega$-meson is used to describe the density dependence of the symmetry energy. A comparison is made between the crust-core transition properties of neutron stars obtained by three different methods, the Relativistic Random Phase Approximation (RRPA), the Vlasov equation and Thermodynamical method. It is shown that the RRPA and the Vlasov methods predict similar transition densities for $pne$ $\beta$-equilibrium stellar matter.

11 pages, 5 figures

References in corpus (17)

• Neutron Star Observations: Prognosis for Equation of State Constraints
• Neutron-Rich Nuclei in Heaven and Earth
• Symmetry Energy I: Semi-Infinite Matter
• Core-crust transition in neutron stars: predictivity of density developments
• Crustal Entrainment and Pulsar Glitches
• Density dependence of the nuclear symmetry energy: a microscopic perspective
• Equation of state and thickness of the inner crust of neutron stars
• Pulsar Glitches: The Crust may be Enough
• Non-rotating and rotating neutron stars in the extended field theoretical model
• The nuclear symmetry energy and stability of matter in neutron star
• The Giant Monopole Resonance in the Sn Isotopes: Why is Tin so "Fluffy"?
• Asymmetric nuclear matter and neutron-skin in extended relativistic mean field model
• Cluster formation in compact stars: relativistic versus Skyrme models
• Low Densities Instability of Relativistic Mean Field Models
• Cluster formation in asymmetric nuclear matter: semi-classical and quantal approaches
• Diversities in the properties of neutron stars at a fixed neutron-skin thickness in ${}^{208}$Pb nucleus
• Shell States of Neutron Rich Matter

Cited by in corpus (16)

• The Vlasov formalism for extended relativistic mean field models: the crust-core transition and the stellar matter equation of state
• Bayesian analysis of the crust-core transition with a compressible liquid-drop model
• Higher-order symmetry energy and neutron star core-crust transition with Gogny forces
• General predictions for the neutron star crustal moment of inertia
• Domains and defects in nuclear "pasta"
• Prior probability distributions of neutron star crust models
• Second and fourth moments of the charge density and neutron-skin thickness of atomic nuclei
• Quantifying the uncertainties on spinodal instability in stellar matter through meta-modeling
• Warm unstable asymmetric nuclear matter: critical properties and the density dependence of the symmetry energy
• Core-crust transition and crustal fraction of moment of inertia in neutron stars
• Nuclear pasta and symmetry energy in the relativistic point-coupling model
• Crust-core interface and bulk neutron star properties
• The symmetry energy $\gamma$ parameter of relativistic mean-field models
• Inner crust of neutron stars with mass-fitted Skyrme interaction
• Hot magnetized nuclear matter: Thermodynamic and Saturation Properties
• Landau parameters and entrainment matrix of cold stellar matter: effect of the symmetry energy and strong magnetic fields