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Magnetic field evolution in magnetars

Published online by Cambridge University Press:  20 March 2013

Yasufumi Kojima
Yasufumi Kojima*
Affiliation:
Department of Physics, Hiroshima University, Higashi-Hiroshima, 739-8526, Japan email: kojima@theo.phys.sci.hiroshima-u.ac.jp
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Abstract

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Dynamics of magnetic field decay is numerically studied. For neutron stars with strong magnetic fields, the Hall drift timescale in their crust is very short, and therefore the evolution is significantly affected. The nonlinear coupling between poloidal and toroidal components of the magnetic field is studied. It is also found that the polar field at the surface is highly distorted during the Hall drift timescale. For example, polar dipole field-strength temporarily decreases not by dissipation but by advection. This fact suggests that the dipole field-strength is not sufficient to determine the border between pulsars and magnetars.

Keywords

magnetic fieldsstars: neutronpulsars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S291: Neutron Stars and Pulsars: Challenges and Opportunities after 80 years , August 2012 , pp. 425 - 427
Copyright
Copyright © International Astronomical Union 2013

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