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Rotation and Magnetic Fields in the Sun

Conference paper

Abstract

Stellar magnetic fields exert torques which, alter the distribution of angular momentum in a star. In the radiative interior of the Sun these torques tend to enforce uniform rotation and the existence of a rapidly rotating core would imply a poloidal field of less than 10–2 G. In the convective envelope magnetic fields generated by dynamo action produce torques which lead to torsional oscillations. A simple nonlinear model allows both multiply periodic and chaotic behaviour. This system demonstrates that both aperiodic magnetic cycles and the irregular modulation responsible for grand minima can be regarded as examples of deterministic chaos. This picture is consistent with the 14C record but implies that the multiply periodic lamination of some Precambrian varves is not associated with the solar cycle.

Keywords

Solar Activity Solar Cycle Convective Zone Differential Rotation Dynamo Model 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer-Verlag Berlin Heidelberg 1987

Authors and Affiliations

  1. 1.Department of Applied Mathematics and Theoretical PhysicsUniversity of CambridgeCambridgeUK

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