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Spectral and photometric variability of the Classical T Tauri stars RY Tauand SU Aur from 2013 to 2022 is analyzed. We find that in SU Aur the H-alphaline's flux at radial velocity RV = -50 +- 7 km/s varies with a period P = 255+- 5 days. A similar effect previously discovered in RY Tau is confirmed withthese new data: P = 21.6 days at RV = -95 +- 5 km/s. In both stars, the radialvelocity of these variations, the period, and the mass of the star turn out tobe related by Kepler's law, suggesting structural features on the disc planeorbiting at radii of 0.2 AU in RY Tau and 0.9 AU in SU Aur, respectively. Bothstars have a large inclination of the accretion disc to the line of sight - sothat the line of sight passes through the region of the disc wind. We proposethere is an azimuthal asymmetry in the disc wind, presumably in the form of'density streams', caused by substructures of the accretion disc surface. Thesestreams cannot dissipate until they go beyond the Alfven surface in the disc'smagnetic field. These findings open up the possibility to learn about thestructure of the inner accretion disc of CTTS on scales less than 1 AU and toreveal the orbital distances related to the planet's formation.

Density streams in the disc winds of Classical T Tauri stars