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 (ξ ≃ 0.05, λ ≃ 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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Dougados, C., Cabrit, S., Ferreira, J. et al. The Origin of Jets from Young Stars: Steady State Disk Wind Models Confronted to Observations. Astrophysics and Space Science 293, 45–52 (2004). https://doi.org/10.1023/B:ASTR.0000044651.96542.23
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DOI: https://doi.org/10.1023/B:ASTR.0000044651.96542.23