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The theory of the scintillation temporal power spectrum and two frequency co-spectrum for radio waves propagating through the near-Sun interplanetary plasma is considered. The relative contributions of the regular motion, turbulent velocity fluctuations and turbulent wave propagation are discussed. The comparison of theory and the known observational data indicates that for distances r < 10R, velocity fluctuations due to large scale Alfvenic waves are most important. For distances 10R < r < 40R, the temporal spectrum is determined by the solar wind motion and slow magnetosonic wave propagation.

Temporal Spectrum of Interplanetary Scintillation in the near-Sun Region.