Generation of a nonaxisymmetric, predominantly toroidal magnetic field in t
he convective layer of the Sun is considered assuming that the process is r
elated to a decrease in the energy consumed for the convective heat transfe
r. It is also assumed that the field is antisymmetric relative to the equat
orial plane and the field strength varies in proportion to the sine or cosi
ne of the azimuthal angle. It is shown that the field strength increases wh
en both a radial gradient of the angular rotation velocity and a steady-sta
te axisymmetric meridional substance circulation are present. A change in t
he direction of the poloidal motion (leading to a change in the overall fie
ld sign) is assumed to take place on attaining a limiting field strength. T
his is probably related to the excitation of the corresponding turbulent me
dium viscosity. In the proposed model, a restart of the field generation pr
ocess is induced by a change in the magnetic field sign. (C) 2001 MAIK "Nau
ka/Interperiodica".