  Spectral and photometric variability of the Classical T Tauri stars RY Tau
and SU Aur from 2013 to 2022 is analyzed. We find that in SU Aur the H-alpha
line'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 with
these new data: P = 21.6 days at RV = -95 +- 5 km/s. In both stars, the radial
velocity of these variations, the period, and the mass of the star turn out to
be related by Kepler's law, suggesting structural features on the disc plane
orbiting at radii of 0.2 AU in RY Tau and 0.9 AU in SU Aur, respectively. Both
stars have a large inclination of the accretion disc to the line of sight - so
that the line of sight passes through the region of the disc wind. We propose
there is an azimuthal asymmetry in the disc wind, presumably in the form of
'density streams', caused by substructures of the accretion disc surface. These
streams cannot dissipate until they go beyond the Alfven surface in the disc's
magnetic field. These findings open up the possibility to learn about the
structure of the inner accretion disc of CTTS on scales less than 1 AU and to
reveal the orbital distances related to the planet's formation.
