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 _ { sym } ) defined at \rho = 0.1 fm ^ { -3 } .