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Dynamo Theory and the Solar Cycle

Published online by Cambridge University Press:  14 August 2015

M. Stix
M. Stix*
Affiliation:
High Altitude Observatory, National Center for Atmospheric Research, † Boulder, Colo. 80303, U.S.A.
*
∗ On leave from Universitäts-Sternwarte, Göttingen, Germany.

Abstract

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In this paper solutions of the mean field induction equation in a spherical geometry are discussed. In particular, the 22-year solar magnetic cycle is considered to be governed by an axisymmetric, periodic solution which is antisymmetric with respect to the equatorial plane. This solution essentially describes flux tubes travelling as waves from mid-latitudes towards the equator. In a layer of infinite extent the period of such dynamo waves solely depends on the strength of the two induction effects, differential rotation and α-effect (cyclonic turbulence). In a spherical shell, however, mean flux must be destroyed by turbulent diffusion, so the latter process might actually control the time scale of the solar cycle.

A special discussion is devoted to the question of whether the angular velocity increases with increasing depth, as the dynamo waves seem to require, or whether it decreases, as many theoretical models concerned with the Sun's differential rotation predict. Finally, theories for the sector structure of the large scale photospheric field are reviewed. These describe magnetic sectors as a consequence of the sectoral pattern in the underlying large scale convection, as non-axisymmetric solutions of the mean field induction equation, or as hydromagnetic waves, modified by rotational effects.

Information

Type
Part 3: Dynamo Theory and Magnetic Dissipation
Information
Symposium - International Astronomical Union , Volume 71: Basic Mechanisms of Solar Activity , 1976, pp. 367 - 388
Copyright
Copyright © Reidel 1976 

Footnotes

†

The National Center for Atmospheric Research is sponsored by the National Science Foundation.

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