Thermal structure of neutron stars with magnetic fields is studied using modern physics input. The relation between the internal (T_int) and local effective surface (T_s) temperatures is calculated and fitted by analytic expressions for magnetic field strengths B from 0 to 10¹⁶ G and arbitrary inclination of the field lines to the surface. The luminosity of a neutron star with dipole magnetic field is calculated and fitted as a function of B, T_int, stellar mass and radius. Finally, we carry out numerical simulations of neutron-star cooling for several models of neutron stars with magnetic fields. We discuss cooling of neutron stars with ultramagnetized envelopes and also the effects of surface magnetic field of the Vela pulsar on possible values of critical temperatures of neutron and proton superfluids in its core.

Page design by Alexander Potekhin (palex.astro@mail.ioffe.ru).
Page created on January 22, 2001.