Statistics – Computation
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...8e..72r&link_type=abstract
Solar and Stellar Activity Cycles, 26th meeting of the IAU, Joint Discussion 8, 17-18 August 2006, Prague, Czech Republic, JD08,
Statistics
Computation
Scientific paper
A new mean-field model for global circulations in convective zones leads to a meridional flow at the base of the convection zone towards the equator with an amplitude of about 7 m/s. This flow is fast enough to realize an advection-dominated alpha-Omega dynamo within the convection zone. The penetration of this flow into the solar tachocline, however, is too weak to play any role in the solar dynamo mechanism. It is sufficient, however, to configure the internal magnetic field of the radiative core so that the tachocline can be explained as a magnetic Hartmann layer due to the existence of a rather weak fossil magnetic field in the solar interior. Also the stability of toroidal magnetic fields in the differentially rotating solar tachocline is important for the dynamo mechanism. The tachocline is a location where the hydrodynamic Rayleigh instability and the magnetic Tayler instability interact. We found stability limits for toroidal fields of only 100 Gauss for an incompressible and stably stratified sphere. The tachocline is thus NOT a suitable site for the storage of too strong magnetic fields. Since the results are based on an extrapolation of the numerical computations, high-resolution calculations for higher magnetic Reynolds numbers and lower magnetic Prandtl numbers are now necessary.
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