Other
Scientific paper
Feb 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003esasp.517...87h&link_type=abstract
In: Proceedings of SOHO 12 / GONG+ 2002. Local and global helioseismology: the present and future, 27 October - 1 November 2002,
Other
3
Solar Convection Zone, Solar Cycle
Scientific paper
Large scale flows within the solar convection zone are thought to be the primary drivers of the Sun's magnetic activity cycle. Differential rotation amplifies the magnetic field and converts poloidal fields into toroidal fields. Poleward meridional flow near the surface carries magnetic flux that reverses the polar magnetic polarities. A deeper, equatorward meridional flow may carry magnetic flux toward the equator. These axisymmetric flows are themselves driven by large scale convective motions. Given these intimate connections between the large scale flows and solar activity, it would be surprising if there were not solar cycle variations in the flow characteristics. Some variations, namely the torsional oscillations, are well established. Other variations, namely changes in the meridional flow and in the shear at the base of the convection zone, are more controversial. In this paper I describe the observed characteristics of the solar cycle and the large scale flows and discuss the nature of the solar cycle variations.
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