On Cooling of Magnetized Neutron Stars

Cooling of neutron stars with dipole magnetic fields is simulated using a realistic model of the anisotropic surface temperature distribution produced by magnetic fields. Suppression of the electron thermal conductivity of outer stellar layers across the field increases thermal isolation of these layers near the magnetic equator. Enhancement of the radiative and longitudinal electron thermal conductivities in quantizing magnetic fields reduces thermal isolation near the magnetic poles. The equatorial increase of the isolation is pronounced for $B \ga 10^{10}$ G, while the polar decrease -- for $B \ga 10^{12}$ G. The effects compensate partly each other, and the actual influence of the magnetic fields on the cooling is weaker than predicted by the traditional theories where the equatorial effects have been neglected.
Comment: LaTeX, 8 pages + 7 Postscript figures, uses l-aa.sty, accepted for publications in Astron. & Astrophys