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On the non-symmetric solar dynamo

  • The Sun:Structure Oscillations, Magnetic Cycle, Surface Variations
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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.

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Authors and Affiliations

  1. Konkoly Observatory, Budapest, Hungary

    I. K. Csada

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  1. I. K. Csada
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Proceedings of the 14th ESLAB Symposium on Physics of Solar Variations, 16–19 September 1980, Scheveningen, The Netherlands.

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Csada, I.K. On the non-symmetric solar dynamo. Sol Phys 74, 103–105 (1981). https://doi.org/10.1007/BF00151278

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  • DOI: https://doi.org/10.1007/BF00151278

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