Wind/Jet Formation in T Tauri Stars: Theory vs. UV Observations
Ana Ine Gomez de Castro, Eva Verdugo, Constantino Ferro-Fontan

Institute: Instituto de Astronomia y Geodesia (CSIC-UCM)>
Institute: ISO Data Center, VILSPA, ESA
Institute: Consejo Superior de Investigaciones Cientificas y Tecnicas (CONICET-Argentina), Universidad de Buenos Aires, Argentina
Contact Email: aig@mat.ucm.es

Abstract: Observations of the base of protostellar jets I carried out with HST-STIS are presented. The Si III] and CIII] profiles are analyzed for 6 T Tauri stars (TTSs). It is found that the line emission is produced in the stellar atmosphere and in the base of the optical jet. The presence of a low density (10e4 - 10e5 cm-3) envelope is detected. High densities (10e10 cm-3) of the line formation region are confirmed for RU Lup. These results are compared with the theoretical predictions of magneto- centrifugal disk winds. It is shown that densities above 10e8 cm-3 cannot be produced by disk winds. The main spectral signature of disk winds is shown to be the presence of asymmetric absorption components in the blue-wing of strong resonance lines. The strength of the components depends on the inclination and on the accretion rate.

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Manuscript submitted: 2001-September-13
"The Future of Cool-Star Astrophysics', 2003, Eds. A. Brown, G. M. Harper, & T. R. Ayres. Proceedings of 12th Cambridge Workshop on Cool Stars, Stellar Systems, & The Sun,
© 2003 University of Colorado.