Speakers
Prof.
Gogi Melikidze
(University of Zielona Gora)Prof.
Janusz Gil
(University of Zielona Gora)Prof.
Ulrich Geppert
(DLR and University of Zielona Gora)
Description
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 $10^4$ 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 $10^{14}$ G and curvature radii of
field lines of about $10^6$ cm, both of which are fundamental for generation of observable radio emission.
Primary author
Prof.
Ulrich Geppert
(DLR and University of Zielona Gora)
Co-authors
Prof.
Gogi Melikidze
(University of Zielona Gora)
Prof.
Janusz Gil
(University of Zielona Gora)
