COOL MASS-LOSING BOUNDARY-LAYERS OF T-TAURI ACCRETION DISKS

We investigate the structure of the boundary layer between a thin accretion disk and a T Tauri star. We solve the one-dimensional hydrodynamical equations in axial symmetry by using the method of matched asymptotic expansions and find steady solutions with significant mass loss and with radiative energy transport into the star. Reprocessing of the radial energy flux in the stellar atmospheric layers.is expected to give rise to the observed ultraviolet and optical continuum flux. The rates of mass-loss and of kinetic energy carried out by the wind are consistent with observations of protostellar and T Tauri winds.