Volume 427, Number 1, November III 2004
|Page(s)||279 - 292|
|Section||Stellar structure and evolution|
|Published online||25 October 2004|
Oscillations of magnetic stars*
II. Axisymmetric toroidal and non-axisymmetric shear Alfvén modes in a spherical shell
Laboratoire d'Astrophysique de Toulouse et Tarbes, Observatoire Midi-Pyrénées, 14 avenue É. Belin, 31400 Toulouse, France e-mail: email@example.com
Accepted: 16 July 2004
We carry out numerical and mathematical investigations of shear Alfvén waves inside of a spherical shell filled with an incompressible conducting fluid, and bathed in a strong dipolar magnetic field. We focus on axisymmetric toroidal and non-axisymmetric modes, in continuation of a previous work by Rincon & Rieutord (2003, A&A, 398, 663). Analytical expressions are obtained for toroidal eigenmodes and their corresponding frequencies at low diffusivities. These oscillations behave like magnetic shear layers, in which the magnetic poles play a key role, and hence become singular when diffusivities vanish. It is also demonstrated that non-axisymmetric modes are split into two categories, namely poloidal or toroidal types, following similar asymptotic behaviours as their axisymmetric counterparts when the diffusivities become arbitrarily small.
Key words: magnetohydrodynamics (MHD) / stars: oscillations / stars: magnetic fields
© ESO, 2004
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