Tachocline, dynamo and the meridional flow connection

Details Tachocline, dynamo and the meridional flow connection Tachocline, dynamo and the meridional flow connection

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007hia....14..293r&link_type=abstract

Highlights of Astronomy, Volume 14, p. 293-294

Astronomy and Astrophysics

Astronomy

Mhd, Turbulence, Sun: Rotation, Sun: Magnetic Fields

Scientific paper

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.

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