Formation of complex rotational structures in convective and isothermal magnetized zones

We study the development of a complex rotation law in the magnetized convec tive and isothermal zones of stars and planetary atmospheres through the de composition of vector quantities in terms of orthogonal vector spherical ha rmonics. In the case of a solar-type extended convective zone, it is assume d that (a) the transformation of thermal into magnetic energy is favorable from the viewpoint of energy balance, (b) the state that is supported with minimum energy loss is realized, and (c) the condition of minimum entropy p roduction consistent with the two previous requirements is satisfied. To fi nd the rotation law of a zone, weak interaction between variations in the r otation and magnetic-field distributions is assumed. Two possible zones of generation of the solar magnetic field are considered. The first is located in the lower half of the solar convective zone and possesses a latitude de pendence of the rotational velocity similar to that observed. The second zo ne is located just below the surface, and has a rotational velocity that de creases sharply with height and depends only weakly on latitude. We also st udy simple equilibrium structures, in particular, those describing the supe r-rotation of the medium in a convective or isothermal zone. Realization of such super-rotation in an isothermal zone is associated with the outflow o f matter and fields toward upper layers. (C) 2001 MAIK "Nauka/Interperiodic a".