  In this work we consider the thermal evolution of rigidly rotating neutron
stars. In order to perform such study we first calculate the structure of
rotating objects, which is considerably more complicated than that of spherical
objects. The structure of rotating neutron stars is obtained by solving
Einstein's equation for a rotationally deformed fluid distributions. The
numerical method used is based on the the KEH. The equation of state used for
computing the neutron star structure and composition is a simple relativistic
mean field model, with parameter set G300. With the structure of rotating
neutron stars computed we calculate the thermal evolution of these objects. In
order to do so, we re-derive the thermal evolution equations to account for the
metric of a rotating object. The cooling of neutron stars with different
frequencies is then calculated. We show that the cooling of the star strongly
depends on the frequency of the object, with higher frequencies stars showing a
substantial temperature difference between the equator and poles.
