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Tachocline, dynamo and the meridional flow connection

Published online by Cambridge University Press:  01 August 2006

Günther Rüdiger
Günther Rüdiger*
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam email: gruediger@aip.de
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Abstract

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Our model for global circulations in the solar convective zone leads to an equatorial drift at its base with an amplitude of about 7 m/s. Its penetration into the solar tachocline is too weak to play any role in the solar dynamo. It confines, however, the internal magnetic decay modes to the radiative core so that the tachocline can be explained as a magnetic Hartmann layer. In the tachocline for the toroidal fields the magnetic Tayler instability exists. We found stability limits for toroidal fields of only 100 G.

Keywords

MHDturbulenceSun: rotationSun: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Highlights of Astronomy 14: Highlights of Astronomy , August 2006 , pp. 293 - 294
Copyright
Copyright © International Astronomical Union 2007

References

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Rüdiger, G., Kitchatinov, L. L., & Arlt, R. 2005, A&A (Letters), 444, L53Google Scholar