The paper presents a formal derivation of the dynamo equations describing the generation of largescale magnetic fields by small-scale cyclonic turbulence (or convection) in a rotating fluid body. The derivation is based on the simple approximation that the individual turbulent cells are small and shortlived. The dynamo equations show that large-scale magnetic fields are generated at a very high rate, in periods comparable to the time of nonuniform rotation. The dynamo equations describe the generation of the quasi-steady field of Earth and the migratory field of the Sun, in characteristic times of 10 and 10 years, respectively.
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E. N. Parker (1970) studied this question.