Velocity distribution in a scintillation picture and the jet structure of the solar wind

A connection of the dispersion dependence of scintillation drift velosity V(ω) with the distribution of the solar wind velocities phi(v) is studied. A case of an arbitrary PHI(V) distribution is considered. The PHI(V) distribution is characterized by a considerable spread of velocities, a sharp decrease in the high-velocity region and by a considerable contribution of the low-velocity region. The results confirm the model with jet structure of the solar wind, where considerable large-scaled variations of velocities and plasma densities are present at the line of sight