  We study different stages of the neutron star cooling by computing neutron
star properties at various temperatures and entropies using an effective chiral
model including hadronic and quark degrees of freedom. Macroscopic properties
of the star such as mass and radius are calculated and compared with
observations. It can be seen that the effects of chiral restoration and
deconfinement to quark matter in the core of the neutron star at different
stages of the evolution can be significant for the evolution of the star and
allow insight into the behaviour of matter at extreme densities.
