  The Vlasov formalism is extended to relativistic mean-field hadron models
with non-linear 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 1.4 $M_\odot$
star.
