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The Solar Dynamo

Published online by Cambridge University Press:  12 April 2016

Axel Brandenburg  and
Ilkka Tuominen
Axel Brandenburg
Affiliation:
Observatory and Astrophysics Laboratory, University of Helsinki, Tähtitorninmäki, SF-00130 Helsinki, Finland NORDITA, Blegdamsvej 17, DK-2100 Copenhagen, Denmark
Ilkka Tuominen
Affiliation:
Observatory and Astrophysics Laboratory, University of Helsinki, Tähtitorninmäki, SF-00130 Helsinki, Finland

Abstract

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The traditional αΩ-dynamo as a model for the solar cycle has been successful in explaining the butterfly diagram, phase relations between poloidal and toroidal field, and polar branch migration features. Observational and theoretical achievements in recent years have however shaken this picture. The current trend is towards dynamos operating in the overshoot region of the convection zone. Nevertheless, there are many open questions and a consistent picture has not been established. In this paper we compare recent approaches and discuss remaining problems.

Type
Part III Solar magnetism and large-scale flows
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 223 - 233
Copyright
Copyright © Springer-Verlag 1991

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