THE GLOBAL SOLAR MAGNETIC-FIELD AS A CONTROLLER FOR THE ORIGIN AND ACCELERATION MODEL OF SOLAR-WIND STREAMS

The 3-D MHD analytical solution as a model of the supersonic transalfvenic solar wind for the low and middle heliolatitudes at a distance of (5-20) solar radii is constructed. The solution shows that typical high-speed stream velocities observed in interplanetary space could be achieved after the flow passes through the transalfvenic region. Relatively small (5%) latitudinal or/and longitudinal magnetic variations arising in the subalfvenic region can cause great (100%) latitudinal or/and longitudinal solar wind velocity variations in the superalfvenic region and play a role of a ''function of control'' for the process of the high-speed stream acceleration. The conditions are indicated under which the areas of local deceleration inside of the flow could exist.