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

Cooling curves for neutron stars with hadronic matter and quark matter