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Additional resources for Accretion Disks and Magnetic Fields in Astrophysics: Proceedings of the European Physical Society Study Conference, Held in Noto (Sicily), Italy, June 16–21, 1988
4. Mean Field Dynamo Theory Most attempts to describe solar and stellar magnetic fields have relied on simplified dynamo models with azimuthally averaged properties. Then we can separate the magnetic field B into poloidal and toroidal components by writing B=Bp+BT, 18 where X A A A Bp = curl (A/fo) = curl (-/fo) , BT = Bq,/fo , s with (s, 1/>, z) cylindrical polar coordinates and ~ a unit vector in the I/>-direction. , cur! /fo - 24>/0 . g. Cowling 1976) shows that a steady axisymmetric field cannot be maintained.
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