Dynamical Instabilities in Relativistic Mean-Field Models and Inner Edge of the Compact Star Crust

We take a dynamical spinodal approach to study the effects of different nuclear relativistic models on the instability zone of nuclear matter in beta equilibrium under the conditions expected to be found in the crust of neutron stars. In particular, we probe the predictive power of those models in the description of the inner edge of the crust. Pressure and the liquid-gas phase densities are evaluated and compared to the most recent "pasta" phase results obtained with a Thomas-Fermi approach for the pasta phases. The collective response from n, p matter is also briefly commented.