The stability of poloidal magnetic fields in rotating stars
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Publication:5427175
DOI10.1051/0004-6361:20065903zbMATH Open1132.85001arXiv0705.0185OpenAlexW2106855464WikidataQ68855009 ScholiaQ68855009MaRDI QIDQ5427175
Author name not available (Why is that?)
Publication date: 19 November 2007
Published in: (Search for Journal in Brave)
Abstract: The stability of large-scale magnetic fields in rotating stars is explored, using 3D numerical hydrodynamics to follow the evolution of an initial poloidal field. It is found that the field is subject to an instability, located initially on the magnetic equator, whereby the gas is displaced in a direction parallel to the magnetic axis. If the magnetic axis is parallel to the rotation axis, the rotation does not affect the initial linear growth of the instability, but does restrict the growth of the instability outside of the equatorial zone. The magnetic energy decays on a timescale which is a function of the Alfv'en crossing time and the rotation speed, but short compared to any evolutionary timescale. No evidence is found for a possible stable end state to evolve from an initial axisymmetric poloidal field. The field of an oblique rotator is similarly unstable, in both cases regardless of the rotation speed.
Full work available at URL: https://arxiv.org/abs/0705.0185
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