T Tauri winds
1981; IOP Publishing; Volume: 244; Linguagem: Inglês
10.1086/158691
ISSN1538-4357
Autores Tópico(s)Solar and Space Plasma Dynamics
Resumoview Abstract Citations (198) References (38) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS T Tau winds. Decampli, W. M. Abstract 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. Publication: The Astrophysical Journal Pub Date: February 1981 DOI: 10.1086/158691 Bibcode: 1981ApJ...244..124D 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; Astrophysics full text sources ADS | data products SIMBAD (21)
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