Alpha-Effect and Turbulent Pumping In The Rapid Rotation Regime - Implications For Solar Dynamo Models

Details Alpha-Effect and Turbulent Pumping In The Rapid Rotation Regime - Implications For Solar Dynamo Models Alpha-Effect and Turbulent Pumping In The Rapid Rotation Regime - Implications For Solar Dynamo Models

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...8e..46k&link_type=abstract

Solar and Stellar Activity Cycles, 26th meeting of the IAU, Joint Discussion 8, 17-18 August 2006, Prague, Czech Republic, JD08,

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We use local 3D convection calculations to compute the alpha-effect and turbulent pumping of mean magnetic fields in the rapid rotation regime corresponding to the deep layers of the solar convection zone. We find that in this regime the alpha-effect responsible for generating the poloidal field out of the toroidal one peaks at around latitude 30 degrees, in contrast to the slow rotation case and the often adopted prescription in mean-field models of the solar dynamo, where the maximum values are found at the poles. Furthermore, the turbulent pumping of mean fields is predominantly down- and equatorward. We find that the downward pumping is decreased near the equator for rapid rotation and can be upward for the toroidal field component. In order to investigate the implications of the obtained local results for the problems in mean-field dynamo theory arising from the helioseismically determined solar rotation profile, namely the poleward migration of activity belts at low latitudes and the activity being concentrated at too high latitudes, we introduce the alpha-effect and turbulent pumping as they were found in the local calculations into a kinematic mean-field model of the solar dynamo. We also investigate the effect of a one-cell counter-clockwise meridional flow pattern on the dynamo solutions. We find that using the alpha-effect and turbulent pumping adapted from the results of the local calculations, the migration of the activity belts is equatorward also at low latitudes. When the meridional flow is added, the activity belts are shifted further closer to the equator, and a poleward migration belt appears at high latitudes. With all the effects included, the activity still appears at too high latitudes (5...60 degrees). Other remaining problems include the somewhat too short cycle periods for the solar-like dipole solutions.

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