Abstract
Spectroscopy of the infrared He I (10830 A) line with NIRSPEC on Keck and CSHELL at the IRTF, and of the ultraviolet C III (977 A) and O VI (1032 A) 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-1), hot (~300,000 K) accelerating outflow with a mass-loss rate ~10-11 to 10-12 M☉ yr-1 or larger. Spectra of T Tau 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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