  A hadronic chiral SU(3) model is applied to neutron and proto-neutron stars,
taking into account trapped neutrinos, finite temperature and entropy. The
transition to the chirally restored phase is studied and global properties of
the stars like minimum and maximum masses and radii are calculated for
different cases. In addition, the effects of rotation on neutron star masses
are included and the conservation of baryon number and angular momentum
determine the maximum frequencies of rotation during the cooling.
