A Hot Wind from the Classical T Tauri Stars: TW Hydrae and T Tauri

Details A Hot Wind from the Classical T Tauri Stars: TW Hydrae and T Tauri A Hot Wind from the Classical T Tauri Stars: TW Hydrae and T Tauri

2005-05-02

arxiv.org/abs/astro-ph/0505037v1

Astrophys.J. 625 (2005) L131-L134

Astronomy and Astrophysics

Astrophysics

To be published in: Astrophysical Journal Letters; 9 pages, 3 figures

Scientific paper

10.1086/431323

Spectroscopy of the infrared He I (10830A) line with KECK/NIRSPEC and IRTF/CSHELL, and of the ultraviolet C III (977A) and O VI (1032A) emission with FUSE reveals that the classical T Tauri star TW Hydrae exhibits P Cygni profiles, line asymmetries, and absorption indicative of a continuous, fast (~400 km/s), hot (~300,000 K) accelerating outflow with a mass loss rate \~10^-11 - 10^-12 solar masses per year, or larger. Spectra of T Tauri N appear consistent with such a wind. The source of the emission and outflow seems restricted to the stars themselves. Although the mass accretion rate is an order of magnitude less for TW Hya than for T Tau, the outflow reaches higher velocities at chromospheric temperatures in TW Hya. Winds from young stellar objects may be substantially hotter and faster than previously thought.

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