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The Case for a Distributed Solar Dynamo Shaped by Near-Surface Shear

© 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A.
, , Citation Axel Brandenburg 2005 ApJ 625 539 DOI 10.1086/429584

0004-637X/625/1/539

Abstract

Arguments for and against the widely accepted picture of a solar dynamo being seated in the tachocline are reviewed, and alternative ideas concerning dynamos operating in the bulk of the convection zone, or perhaps even in the near-surface shear layer, are discussed. Based on the angular velocities of magnetic tracers, it is argued that the observations are compatible with a distributed dynamo that may be strongly shaped by the near-surface shear layer. Direct simulations of dynamo action in a slab with turbulence and shear are presented to discuss filling factor and tilt angles of bipolar regions in such a model.

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10.1086/429584