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 $(L,K_{\mathrm{sym}})$ defined at $\rho =0.1$ fm${}^{-3}$.

• Received 2 February 2011

DOI:https://doi.org/10.1103/PhysRevC.83.045810