Dynamo Action in the Solar Convection Zone and Tachocline: Pumping and Organization of Toroidal Fields

Details Dynamo Action in the Solar Convection Zone and Tachocline: Pumping and Organization of Toroidal Fields Dynamo Action in the Solar Convection Zone and Tachocline: Pumping and Organization of Toroidal Fields

2006-09-06

arxiv.org/abs/astro-ph/0609153v1

Astrophys.J.648:L157-L160,2006

Astronomy and Astrophysics

Astrophysics

4 pages, 3 color figures (compressed), in press at ApJL

Scientific paper

10.1086/507869

We present the first results from three-dimensional spherical shell simulations of magnetic dynamo action realized by turbulent convection penetrating downward into a tachocline of rotational shear. This permits us to assess several dynamical elements believed to be crucial to the operation of the solar global dynamo, variously involving differential rotation resulting from convection, magnetic pumping, and amplification of fields by stretching within the tachocline. The simulations reveal that strong axisymmetric toroidal magnetic fields (about 3000 G in strength) are realized within the lower stable layer, unlike in the convection zone where fluctuating fields are predominant. The toroidal fields in the stable layer possess a striking persistent antisymmetric parity, with fields in the northern hemisphere largely of opposite polarity to those in the southern hemisphere. The associated mean poloidal magnetic fields there have a clear dipolar geometry, but we have not yet observed any distinctive reversals or latitudinal propagation. The presence of these deep magnetic fields appears to stabilize the sense of mean fields produced by vigorous dynamo action in the bulk of the convection zone.

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