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T Tauri winds
Decampli, W. M.
Astrophysical Journal, Part 1, vol. 244, Feb. 15, 1981, p. 124-146. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Magnetohydrodynamic Waves, Stellar Mass Ejection, Stellar Winds, T Tauri Stars, Astronomical Spectroscopy, H Alpha Line, H Beta Line, Radial Velocity, Radiation Pressure, Stellar Magnetic Fields, Stellar Models, Stellar Rotation
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The problem of mass loss from T Tauri stars is addressed. It is shown that, as deduced from the H-alpha line intensity alone, the mass loss rates from the 'average' T Tauri star have an ambiguity of at least three orders of magnitude. In the case of mass loss rates less than approximately 10 to the -9th solar mass per year, thermal coronal expansion or line radiation pressure is considered a possible wind mechanism. For rates between 10 to the -9th and a few x 10 to the -8th solar mass per year, the deposition of the momentum of Alfven waves generated in a convection zone is thought to be a plausible mechanism. A model is presented in which a rotating star has a wind driven by this mechanism, and simplified examples are displayed. No acceptable mechanism is found in the 'average' T Tauri star for maintaining a wind with strength greater than a few x 10 to the -8th solar mass per year.

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Database: Astronomy
arXiv e-prints