Dissipation of magnetic fields in neutron star crusts due to development of a tearing mode
Abstract
Dissipation of magnetic fields in Hall plasma of neutron star crusts may power persistent high energy emission of a class of strongly magnetized neutrons stars, magnetars. We consider development of a dissipative tearing mode in Hall plasma (electron MHD) and find that its growth rate increases with the wave number of perturbations, reaching a maximum value intermediate between resistive τr and Hall times τH, 1 / τr τH. We argue that the tearing mode may be the principal mechanism by which strong magnetic fields are dissipated in magnetars on times scale of 104-105 yrs powering the persistent X-ray emisison.
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