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Magnetohydrodynamic processes in strongly magnetized young neutron stars

Lookup NU author(s): Dr Vadim Urpin


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We examine the early evolution of a neutron star with a very strong magnetic field (B ≥ 4 × 1013 G) that occupies a significant fraction of the core volume. The electrical conductivity of the core matter is a strong function of the magnetic field, therefore the evolution of magnetized neutron stars (magnetars) may well be different from that of ordinary radiopulsars. We consider magnetohydrodynamic processes in the core for two possible models of nuclear matter, with normal and superfluid neutrons. In the case of the normal matter, an enhancement of the resistivity perpendicular to the magnetic field can result in rapid field decay during the early evolutionary stage. If neutrons are in the superfluid state, we find that the Hall effect can lead to oscillatory behaviour of the magnetic field. This oscillatory behaviour is caused by the generation of large-scale helicoid modes resulting from non-linear coupling between the different field components.

Publication metadata

Author(s): Urpin V, Shalybkov D

Publication type: Article

Publication status: Published

Journal: Monthly Notices of the Royal Astronomical Society

Year: 1999

Volume: 304

Issue: 2

Pages: 451-456

Print publication date: 01/04/1999

ISSN (print): 0035-8711

ISSN (electronic): 1365-2966

Publisher: Wiley-Blackwell Publishing Ltd.


DOI: 10.1046/j.1365-8711.1999.02341.x


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