  The thermal evolution of isothermal neutron stars is studied with matter both
in the hadronic phase as well as in the mixed phase of hadronic matter and
strange quark matter. In our models, the dominant early-stage cooling process
is neutrino emission via the direct Urca process. As a consequence, the cooling
curves fall too fast compared to observations. However, when superfluidity is
included, the cooling of the neutron stars is significantly slowed down.
Furthermore, we find that the cooling curves are not very sensitive to the
precise details of the mixing between the hadronic phase and the quark phase
and also of the pairing that leads to superfluidity.
