The Origin of Jets from Young Stars: Steady State Disk Wind Models Confronted to Observations

Details The Origin of Jets from Young Stars: Steady State Disk Wind Models Confronted to Observations The Origin of Jets from Young Stars: Steady State Disk Wind Models Confronted to Observations

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004ap%26ss.293...45d&link_type=abstract

Astrophysics and Space Science, v. 293, Issue 1, p. 45-52 (2004).

Astronomy and Astrophysics

Astrophysics

8

T Tauri Stars, High-Angular Resolution, Jets, Magneto-Hydrodynamic

Scientific paper

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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