Radio pulsar activity and the crustal Hall drift
arXiv:1308.2718 · doi:10.1093/mnras/stt1527
Abstract
Models of pulsar radio emission that are based on an inner accelerating region require the existence of very strong and small scale surface magnetic field structures at or near the canonical polar cap. The aim of this paper is to identify a mechanism that creates such field structures and maintains them over a pulsar's lifetime. The likely physical process that can create the required 'magnetic spots' is the Hall drift occurring in the crust of a neutron star. It is demonstrated, that the Hall drift can produce small scale strong surface magnetic field anomalies (spots) on timescales of years by means of non-linear interaction between poloidal and toroidal components of the subsurface magnetic field. These anomalies are characterized by strengths of about G and curvature radii of field lines of about cm, both of which are fundamental for generation of observable radio emission.
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Cited by in corpus (26)
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- Three-dimensional simulations of the magnetic stress in a neutron star crust
- Radio efficiency of pulsars
- Hall drift and the braking indices of young pulsars
- Two Modes of Partially Screened Gap
- Creation of magnetic spots at the neutron star surface
- The Nature of Coherent Radio Emission from Pulsars
- A deep campaign to characterize the synchronous radio/X-ray mode switching of PSR B0943+10
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- Gravitational radiation from neutron stars deformed by crustal Hall drift
- Density-shear instability in electron MHD
- Rapid Modification of Neutron Star Surface Magnetic Field: A proposed mechanism for explaining Radio Emission State Changes in Pulsars
- A Single spark model for PSR J21443933
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- On the Origin of Radio Emission from Magnetars
- Heating of the Real Polar Cap of Radio Pulsars
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- Linear-drifting sub-pulse sources in radio pulsars
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- Synchrotron X-ray emission from old pulsars