The Vlasov formalism is extended to relativistic mean field hadron models with nonlinear terms up to fourth order and applied to the calculation of the crust-core transition density. The effect of the nonlinear $\omega \rho$ and $\sigma \rho$ coupling terms on the crust-core transition density and pressure and on the macroscopic properties of some families of hadronic stars is investigated. For that purpose, six families of relativistic mean field models are considered. Within each family, the members differ in the symmetry energy behavior. For all the models, the dynamical spinodals are calculated, and the crust-core transition density and pressure and the neutron star mass-radius relations are obtained. The effect on the star radius of the inclusion of a pasta calculation in the inner crust is discussed. The set of six models that best satisfy terrestrial and observational constraints predicts a radius of $13.6\pm 0.3$ km and a crust thickness of $1.36\pm 0.06$ km for a $1.4M_{\odot }$ star.

• Received 3 March 2016
• Revised 27 May 2016

DOI:https://doi.org/10.1103/PhysRevC.94.015808