Abstract
The solar dynamo problem is reviewed in the light of recent developments in dynamo theory. We distinguish between the generation of magnetic fields on scales smaller than the velocity correlation length-small scale dynamo, and larger than the velocity correlation length-large scale dynamo. We argue that small scale dynamo action is likely to occur everywhere in the convection zone. The field thus generated however is disordered both in space and time. Large scale dynamo action on the other hand is responsible for the activity cycle and the large scale organization of the solar field. The existence of a large scale dynamo is related to the breaking of symmetries in the underlying field of turbulence.
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