Magnetization and nature of the rotation of the solar convective zone

An analysis is made of adiabatic magnetized differentially rotating structures of the stellar convective zone obtained by minimizing the production of entropy. The change in the law of rotation when one type of magnetic field is replaced by another (for example, a toroidal field by a poloidal one) is studied. It is found that for the latitude distribution of the rotation observed on the Sun, the variation in the latitude gradient of the angular rotation speed is comparatively small for this change in fields. This condition facilitates the establishment of cyclic variations in the field. In a configuration in which the equatorial layers rotate faster, it becomes more difficult for these variations to exist, which may account for the well-known Maunder minimum of solar activity.

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