Abstract
We discuss in this contribution constraints on the origin of mass-loss from young stars brought by recent observations at high angular resolution (0.1″=14 AU) of the inner regions of winds from T Tauri stars. Jet widths and collimation scales, the large extent of the velocity profile as well as the detection of rotation signatures agree with predictions from extended (R e ≥ 1 AU) magneto-centrifugal disk wind ejection models. Detected poloidal and toroidal velocities imply large ejection efficiencies (\(\xi \simeq 0.05,\lambda \simeq 10\)), suggesting that thermal gradients (originating in an accretion heated disk corona for example) play an important role in accelerating the flow.
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