Jets from T Tauri stars - spectroscopic evidence and collimation mechanism

Journal Article · Thu Sep 01 04:00:00 EDT 1988 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/185262· OSTI ID:7051642

Kwan, J; Tademaru, E

Based upon analysis of observed O I (6300 A) forbidden line profiles, it is argued that two separate gas components contribute to the forbidden line emission from T Tauri stars. There is a high-speed component due to a wind from the star, and a low-speed component due to a wind from the circumstellar disk and/or a warm disk corona. Further, most of the high-speed gas particles have velocity vectors nearly parallel to one another, indicating a well-collimated flow. The collimation of an initially radially expanding wind is ascribed to the effect of the magnetic field produced by currents in the circumstellar disk. Assuming that this magnetic field is roughly parallel to the stellar rotation axis, the stellar wind will be collimated into bipolar jets. It is estimated that the disk radius is about 100 AU, the disk magnetic field is about 0.1 G, and the stellar mass-loss rate is about 10 to the -7th solar masses/yr. The orientation of the disk can be deduced from the velocity displacement of the jet emission from the stellar rest velocity. 11 references.

• Research Organization: Massachusetts Univ., Amherst (USA)
• OSTI ID: 7051642
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 332; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
COSMIC RADIO SOURCES
EMISSION SPECTRA
ERUPTIVE VARIABLE STARS
MAGNETIC FIELDS
MASS
MASS TRANSFER
MOTION
PLASMA JETS
ROTATION
SPECTRA
STARS
STELLAR ACTIVITY
STELLAR WINDS
T TAURI STARS
VARIABLE STARS
VELOCITY