Wind/jet Formation in T Tauri Stars: Theory versus UV Observations

Details Wind/jet Formation in T Tauri Stars: Theory versus UV Observations Wind/jet Formation in T Tauri Stars: Theory versus UV Observations

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003csss...12...40g&link_type=abstract

The Future of Cool-Star Astrophysics: 12th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (2001 July 30 - August

Astronomy and Astrophysics

Astrophysics

2

T Tau, De Tau, Ru Lup, Rw Aur, Ak Sco, Ry Tau, Hst/Stis, Disk Wind Models

Scientific paper

Observations of the base of protostellars jet carried out with HST-STIS are presented. The Si III] and CIII] profiles are analized 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 (104-105 cm-3) envelope is detected. High densities (˜ 1010 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 108 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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