In this special issue article, I review some of the accomplishments of the
chiral mean field (CMF) model, which contains nucleon, hyperon, and quark
degrees of freedom, and its applications to proto-neutron and neutron stars. I
also present a set of equation of state and particle population tables built
using the CMF model subject to physical constraints necessary to reproduce
different environments, such as those present in cold neutron stars,
core-collapse supernova explosions and different stages of compact star
mergers.Comment: PASA special issue on the Neutron Stars, related to the Compstar
conference in Warsa