On the Dynamo Action of the Global Convection in the Solar Convection Zone

Abstract

The very large-scale nonaxisymmetric convection in the solar convection zone, called here the global convection, has been conceived to explain the solar equatorial acceleration, the clustering in longitudes of magnetic activities, and the proper motions of sunspots. The magnetohydrodynamics of the convection is examined in the framework of a slowly rotating spherical geometry, and the dynamo action is shown to be operated by the global convection when modified by rotation in such a way as to regenerate and reverse the poloidal general magnetic field in the middle layer in the solar convection zone. The global convection driven by the convective instability, in this way, is the basic driving power of both the solar differential rotation and the cyclic magnetic activities of the Sun, i.e., the solar cycle.