Various possibilities of the structure of the magnetic field, which is driven by turbulent dynamo mechanisms, in the stellar convection zone are analysed, putting an emphasis on the cross-helicity dynamo effect. A relation between the cross-helicity dynamo and rotation is discussed. An evaluation is made for the cross-helicity-driven magnetic field, and the influence of the rotation is illustrated. A case in which the convection zone is lying just below the surface (like the solar convection zone) is analysed. The toroidal magnetic field structure is predicted to exist in stellar interior, and the analogy to laboratory toroidal plasmas is explained. The interior magnetic field is divided into two classes. One is dominated by the poloidal–radial component: activity may be seen near the polar region for this case. In the other, the magnetic field is dominated by the toroidal magnetic field as tokamaks in laboratory experiments.
Axisymmetric two-fluid plasma equilibria with momentum sources and sinks