Abstract
Using statistics of sunspot group proper motions, the behaviour of differential rotation in the solar convection zone is investigated. It can be argued that young groups, during the first days after their appearance at the solar surface, carry information on the motions deep in the convection zone. This gives a possibility of probing both the radial dependence of the differential rotation and its latitudinal profile, which are basic constraints for the solar dynamo. The results indicate that the angular velocity increases in the lower part of the convection zone. The temporal variation of the rotation is consistent with this picture. The profile of latitudinal differential rotation varies following the solar cycle, but is in opposite phase at the surface and deep in the convection zone. This is in accordance with our predictions, if the variations are produced by a back-reaction of the dynamo magnetic fields.
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