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The possibility to draw links between the isospin properties of nuclei andthe structure of compact stars is a stimulating perspective. In order to pursuethis objective on a sound basis, the correlations from which such links can bededuced have to be carefully checked against model dependence. Using a varietyof nuclear effective models and a microscopic approach, we study the relationbetween the predictions of a given model and those of a Taylor densitydevelopment of the corresponding equation of state: this establishes to whatextent a limited set of phenomenological constraints can determine thecore-crust transition properties. From a correlation analysis we show that a)the transition density $\rho_t$ is mainly correlated with the symmetry energyslope $L$, b) the proton fraction $Y_{p,t}$ with the symmetry energy andsymmetry 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 transitionpressure $P_t$ with the symmetry energy slope and curvature $(J,K_{\rm sym})$defined at $\rho=0.1$ fm$^{-3}$.

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