Abstract
Abstract We consider a decay of the magnetic field, originally confined to a moderately deep layer of the neutron star crust with the density ρ ≲ 4 · 1011 g/cm3. The effect of neutron star cooling on the conductivity and the rate of the magnetic field dissipation is taken into account. The main goal of this paper is the investigation of the influence of the field decay on the neutron star spinning down in the magnetic dipole braking model. Evolutionary tracks of pulsars on the B s – P diagram, where B s is the magnetic field at the surface and P is the spin period, have been calculated. It is shown that the crustal decay model is in a qualitative agreement with observational data if a significant fraction of the outer crust was originally occupied by the magnetic field.
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