Dissipation of magnetic fields in neutron star crusts due to development of a tearing mode
| dc.creator | Lyutikov, Maxim | |
| dc.date | 2007-05-22 | |
| dc.date.accessioned | 2026-07-07T08:02:52Z | |
| dc.date.available | 2026-07-07T08:02:52Z | |
| dc.description | 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 $τ_r$ and Hall times $τ_H$, $Γ\sim 1 / \sqrt{τ_r τ_H}$. 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. | |
| dc.description | 10 pages | |
| dc.identifier | https://arxiv.org/abs/0705.3186 | |
| dc.identifier | http://arxiv.org/abs/0705.3186 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/129367 | |
| dc.subject | Astrophysics | |
| dc.title | Dissipation of magnetic fields in neutron star crusts due to development of a tearing mode | |
| dc.type | text |