Statistical analysis of spatial velocity distributions in the solar wind in scintillations

Investigations into a space structure of the solar wind using the dispersion scintillation analysis have been carried on. Specific features of the space structure of velocities in the solar wind have been studied depending on heliocentric latitude and a form of the velocity distribution function. During the analysis used were data on scintillation observations at great distances from the Sun, R>=0.4 a.u, at 74 MHz obtained at the California University Observatory. The presence in the solar wind of different modes of plasma outflow depending on effective velocity of plasma inhomogeneities is concluded less stable during slow plasma outflow and more stable during fast plasma outflow