A study of the kinematics of the H2O maser sources S269 and W75S from long-term monitoring

It is shown that basic characteristics of turbulence can be derived from te mporal behaviour, shape and radial-velocity drift of a spectral line. To pe rform this analysis, a 20-year monitoring of the H2O maser emission sources S269 and W75S was used. It is shown that the observed sinusoidal variation of the radial velocity of the main emission feature in S269 with a period of 26 years is not caused by Keplerian motion. Most likely, it results from rotation of a non-uniform turbulent vortex with a diameter of about 1 AU. Within the framework of this model, asymmetry of the emission feature at 20 .1 km s(-1) and a jump of the linewidth, which took place after a strong ar e in 1991, are explained. In W75S anticorrelation between fluxes of several emission features with close radial velocities is found. This anticorrelat ion is explained by competition of spatial modes of the emission for pumpin g in a partially saturated maser. It is shown that in the model of a maser in an expanding envelope (which is, most likely, the case in W75S) the emis sion features with anticorrelated fluxes form a spatially compact group.