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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 $(L,K_{\rm sym})$ defined at $\rho=0.1$ fm$^{-3}$.
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Submitted on : Friday, May 20, 2011 - 1:11:07 PM
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Camille Ducoin, Jérôme Margueron, Constança Providência, Isaac Vidaña. Core-crust transition in neutron stars: predictivity of density developments. Physical Review C, American Physical Society, 2011, 83, pp.045810. ⟨10.1103/PhysRevC.83.045810⟩. ⟨in2p3-00562046v2⟩

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