  The critical properties for the transition to warm, asymmetric,
non-homogeneous nuclear matter are analysed within a thermodynamical spinodal
approach for a set of well calibrated equations of state. It is shown that even
though different equations of state are constrained by the same experimental,
theoretical and observational data, and the properties of symmetric nuclear
matter are similar within the models, the properties of very asymmetric nuclear
matter, such as the one found inside of neutron stars, differ a lot for various
models. Some models predict larger transition densities to homogeneous matter
for beta-equilibrated matter than for symmetric nuclear matter. Since one
expects that such properties have a noticeable impact on the the evolution of
either a supernova or neutron star merger, this different behavior should be
understood in more detail.
