A HOT WIND FROM THE CLASSICAL T TAURI STARS: TW HYDRAE AND T TAURI

摘要

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) solar mass 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.