The properties of the core-crust transition in neutron stars are investigated
using effective nuclear forces of finite-range. Special attention is paid to the
so-called dynamical method for locating the transition point, which, apart from the stability of the uniform nuclear matter against clusterization, also considers contributions due to finite-size effects.In particular, contributions to the transition density and pressure from the direct and exchange energies are carefully analyzed. To this end, finite-range forces of Gogny, Momentum-Dependent
Interaction (MDI) and Simple Effective Interaction (SEI) types are used in the numerical applications. The results from the dynamical approach are compared with those from the popular thermodynamical method that neglects the surface and Coulomb effects in the stability condition.In the particular case of the D1M and D1M$^*$ Gogny forces, the core-crust transition density and pressure are also compared with the estimate obtained from the crust side making use of a recently calculation of the Equation of State in the inner crust performed with these Gogny interactions.The dependence of the core-crust transition on the stiffness of the symmetry energy of the finite-range models i also addressed. Finally, we analyze the impact of the transition point on the mass, thickness and fraction of the moment of inertia of the neutron star. Prominent differences in these crustal properties of the star are found between using the transition point obtained with the dynamical method or the thermodynamical method. It is concluded that the core-crust transition needs to be ascertained as precisely as possible in order to have realistic estimates of the observed phenomena where the crust plays a significant role.