Physics
Scientific paper
Sep 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989esoc...33..385e&link_type=abstract
ESO Workshop on Low Mass Star Formation and Pre-Main Sequence Objects, p. 385 - 397
Physics
17
T Tauri Stars: Stellar Winds, T Tauri Stars: P Cygni Profiles, T Tauri Stars: Circumstellar Disks, T Tauri Stars: Accretion, T Tauri Stars: Mass Loss
Scientific paper
The authors argue that energetic T Tauri winds diagnosed by broad blueshifted forbidden emission lines and by P Cygni-like Hα profiles derive their energy from a source external to the star. This energy reservoir is likely to be a circumstellar disk in which gravitational potential energy is released as material is accreted through the optically thick inner regions of the disk. A large range of disk accretion rates and resultant wind mass loss rates would then account for the full spectrum of T Tauri activity. In those stars whose disks have become optically thin in their inner regions, there is no longer any signature of an energetic wind, suggesting that in these stars, disk accretion has stopped. The authors also present evidence that collimated jets, ususally associated with outflows from younger, more embedded sources, persist during the T Tauri phase of evolution.
Cabrit Silvie
Edwards S. S.
Ghandour Louma O.
Strom Stephen E.
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