Mass loss in T Tauri stars - Observational studies of the cool parts of their stellar winds and expanding shells

Details Mass loss in T Tauri stars - Observational studies of the cool parts of their stellar winds and expanding shells Mass loss in T Tauri stars - Observational studies of the cool parts of their stellar winds and expanding shells

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...280..749m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 280, May 15, 1984, p. 749-770. Sponsorship: Deutsche Forschungsgemeinschaft

Astronomy and Astrophysics

Astrophysics

123

Pre-Main Sequence Stars, Stellar Evolution, Stellar Mass Ejection, Stellar Spectra, Stellar Winds, T Tauri Stars, Absorption Spectra, H Alpha Line, Radial Velocity, Signal To Noise Ratios

Scientific paper

Extensive high-resolution and high signal-to-noise line profile measurements of 23 T Tauri stars are presented. Those stars showing indications for mass loss in the Na D lines were observed in H-alpha and Ca II K as well. Mass loss in these stars is found to be often indicated in the Na D lines by rather sharp blueshifted absorption lines. The observed line profiles strongly suggest that, at least in some stars, the winds are already accelerated to 150-350 km/s within 1.1-1.5 stellar radii. For the narrow, blueshifted Na D absorptions, two formation regions are discussed: (1) the distant, cold parts of the stellar wind, and (2) a stellar wind-driven shell. The descending material occasionally observed in some T Tauri stars is interpreted to be infalling matter recently ejected by these stars, and not matter left over from the star formation process.

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