Critical properties of calibrated relativistic mean-field models for the transition to warm, nonhomogeneous nuclear and stellar matter
The critical properties for the transition to warm, asymmetric, nonhomogeneous nuclear matter are analyzed 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 β -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.