The penetration of meridional flow into the tachocline and its meaning for the solar dynamo

Details The penetration of meridional flow into the tachocline and its meaning for the solar dynamo The penetration of meridional flow into the tachocline and its meaning for the solar dynamo

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...444l..53r&link_type=abstract

Astronomy and Astrophysics, Volume 444, Issue 3, December IV 2005, pp.L53-L56

Astronomy and Astrophysics

Astrophysics

16

Hydrodynamics, Sun: Interior, Stars: Interiors

Scientific paper

The penetration of meridional flow into the radiative solar interior is computed with a mean-field model for global circulation in convective zones. The results clearly show that the penetration under solar conditions belongs to the Ekman regime. The penetration is too weak to play any role in the solar dynamo mechanism. We argue, however, that this penetration is sufficient to configure the internal magnetic field of the radiative core so that the solar tachocline can be explained as a Hartmann layer. The resulting meridional flow at the base of the convection zone is fast enough (~7 m/s) to realize an advection-dominated αΩ-dynamo within the convection zone.

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