Thermal structure and cooling of neutron stars with magnetized envelopes

The thermal structure of neutron stars with magnetized envelopes is studied using modern physics input. The relation between the internal (Tint) and local surface temperatures is calculated and tted by analytic expressions for magnetic eld strengths B from 0 to 10 16 G and arbitrary inclination of the eld lines to the surface. The luminosity of a neutron star with dipole magnetic eld is calculated and tted as a function of B, Tint, stellar mass and radius. In addition, we simulate cooling of neutron stars with magnetized envelopes. In particular, we analyse ultramagnetized envelopes of magnetars and also the eects of the magnetic eld of the Vela pulsar on the determination of critical temperatures of neutron and proton superfluids in its core.

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