Abstract
The external field of the solar magnetohydrodynamic dynamo is expressed in terms of spherical harmonics and in powers of 1/r. The non-symmetric dynamo is stabilized by a φ -dependent rotational oscillation which interacts with the magnetic field, thus compensating for Ohmic loss. As a consequence, the axis of a dipole wave is found to move on a great circle, with revolution time equal to the magnetic cycle.
Proceedings of the 14th ESLAB Symposium on Physics of Solar Variations, 16–19 September 1980, Scheveningen, The Netherlands.
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© 1981 Springer Science+Business Media Dordrecht
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Csada, I.K. (1981). On the Non-Symmetric Solar Dynamo. In: Domingo, V. (eds) Physics of Solar Variations. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-9633-1_12
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DOI: https://doi.org/10.1007/978-94-010-9633-1_12
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