Accretion and wind modulation in T Tauri star RY Tau: a planet at 0.2 AU?

Spectral and photometric monitoring of CTTS RY Tau in 2013-2021 revealed variations in the H-alpha and NaI D lines at radial velocities of infall (accretion) and out ow (wind) with a period of about 22 days. The NaI D absorption in the infalling and out owing gas changes in anti-phase: an increase in the density of infalling gas is accompanied by a decrease in the wind density, and vice versa. The fluctuations remain coherent for several years of observation. We assume that the observed effect may be due to processes at the disk-magnetosphere boundary in MHD propeller mode. The stability of the oscillation phase indicates the possible presence of a massive planet, causing azimuthal asymmetry of the accretion and wind flows. If the observed period (22 days) is Keplerian, then the planet is located at a distance of 0.2 AU and moves with an orbital velocity of 100 km s^-1.