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Jets, Disk Winds, and Warm Disk Coronae in Classical T Tauri Stars

Published online by Cambridge University Press:  25 May 2016

John Kwan
John Kwan*
Affiliation:
Department of Physics and Astronomy, University of Massachusetts, Amherst, MA 01003, USA

Abstract

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Arguments, based on analysis of the forbidden line emission, are summarized that point to two components of mass ejection in classical T Tauri stars. A low-speed wind originates from the accretion disk at between ∼ 0.05 AU and ≳3 AU from the star, and a high-speed flow, which becomes collimated into a jet within ≲ 100 AU, originates as a wind from either the star or the very inner part of the accretion disk. The [OI] λ5577 emission in the low-speed component also requires the presence of a warm disk corona, with an electron density of ∼ 107 cm–3 and a temperature of ∼ 8000 K. Additional indication of a warm disk corona comes from analysis of the central absorptions seen in the profiles of the hydrogen Balmer lines. The need to heat the disk corona implies that a substantial fraction of the energy released in the accretion of matter through the disk may be dissipated at the disk surface.

Type
IV. Disks, Winds, and Magnetic Fields
Information
Symposium - International Astronomical Union , Volume 182: Herbig-Haro Flows and the Birth of Low Mass Stars , 1997 , pp. 443 - 454
Copyright
Copyright © Kluwer 1997 

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