Dissipation of magnetic fields in neutron star crusts due to development of a tearing mode

Details Dissipation of magnetic fields in neutron star crusts due to development of a tearing mode Dissipation of magnetic fields in neutron star crusts due to development of a tearing mode

2007-05-22

arxiv.org/abs/0705.3186v1

Astronomy and Astrophysics

Astrophysics

10 pages

Scientific paper

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 $\tau_r$ and Hall times $\tau_H$, $\Gamma\sim 1 / \sqrt{\tau_r \tau_H}$. We argue that the tearing mode may be the principal mechanism by which strong magnetic fields are dissipated in magnetars on times scale of $\sim 10^4-10^5$ yrs powering the persistent X-ray emisison.

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