  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.
