Core-crust transition in neutron stars: predictivity of density developments

Abstract

The possibility to draw links between the isospin properties of nuclei and the structure of compact stars is a stimulating perspective. In order to pursue this objective on a sound basis, the correlations from which such links can be deduced have to be carefully checked against model dependence. Using a variety of nuclear effective models and a microscopic approach, we study the relation between the predictions of a given model and those of a Taylor density development of the corresponding equation of state: this establishes to what extent a limited set of phenomenological constraints can determine the core-crust transition properties. From a correlation analysis we show that a) the transition density ${\rho }_t$ is mainly correlated with the symmetry energy slope $L$, b) the proton fraction $Y_{p,t}$ with the symmetry energy and symmetry energy slope $(J,L)$ defined at saturation density, or, even better, with the same quantities defined at $\rho =0.1$ fm${}^{-3}$, and c) the transition pressure $P_t$ with the symmetry energy slope and curvature $(J,K_{\mathrm{sym}})$ defined at $\rho =0.1$ fm${}^{-3}$.

References in corpus (13)

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• Density dependence of the nuclear symmetry energy: a microscopic perspective
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• Incompressibility of neutron-rich matter
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• Cluster formation in compact stars: relativistic versus Skyrme models
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• Spinodal instabilities of asymmetric nuclear matter within the Brueckner--Hartree--Fock approach

Cited by in corpus (15)

• Relativistic Mean-Field Hadronic Models under Nuclear Matter Constraints
• Equation of state and thickness of the inner crust of neutron stars
• Constraining hypernuclear density functional with $\Lambda$-hypernuclei and compact stars
• Neutron skins and neutron stars
• Effects of the symmetry energy on properties of neutron star crusts near the neutron drip density
• Light clusters, pasta phases and phase transitions in core-collapse supernova matter
• Magnetar superconductivity versus magnetism: neutrino cooling processes
• Constraints on the symmetry energy from observational probes of the neutron star crust
• Influence of the symmetry energy on nuclear pasta in neutron star crusts
• Neutron star structure and collective excitations of finite nuclei
• Equation of state of nuclear matter from empirical constraints
• Correlations between the nuclear matter symmetry energy, its slope, and curvature from a nonrelativistic solvable approach and beyond
• Influence of the single-particle structure on the nuclear surface and the neutron skin
• Quantifying Correlations Between Isovector Observables and the Density Dependence of Nuclear Symmetry Energy away from Saturation Density
• Core-crust transition properties of neutron stars within systematically varied extended relativistic mean-field model