Core-crust transition in neutron stars: predictivity of density developmentsReport as inadecuate

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* Corresponding author 1 Centro de Fisica Computacional, University of Coimbra 2 IPNO - Institut de Physique Nucléaire d-Orsay

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 $ ho 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 $ ho=0.1$ fm$^{-3}$, and c the transition pressure $P t$ with the symmetry energy slope and curvature $L,K { m sym}$ defined at $ ho=0.1$ fm$^{-3}$.

Keywords : neutron-star crust symmetry energy nuclear equation of state Skyrme forces relativistic nuclear models Brueckner-Hartree-Fock approach

Author: Camille Ducoin - Jérôme Margueron - Constança Providência - Isaac Vidaña -



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