The case for a distributed solar dynamo shaped by near-surface shear
Astrophysics
2007-05-23 v1
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.
Cite
@article{arxiv.astro-ph/0502275,
title = {The case for a distributed solar dynamo shaped by near-surface shear},
author = {Axel Brandenburg},
journal= {arXiv preprint arXiv:astro-ph/0502275},
year = {2007}
}
Comments
10 pages, 6 figures, Astrophys. J. 625 (scheduled for the 1 June 2005 issue)