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Wave-driven winds from cool stars. II - Models for T Tauri stars
Hartmann, L.; Avrett, E.; Edwards, S.
AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AC(Smith College, Northampton, MA)
Astrophysical Journal, Part 1, vol. 261, Oct. 1, 1982, p. 279-292. Research supported by the Smithsonian Institution; (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Cool Stars, Magnetohydrodynamic Waves, Stellar Winds, T Tauri Stars, Temperature Distribution, Balmer Series, Chromosphere, H Alpha Line, Stellar Mass Ejection, Ultraviolet Spectra
Bibliographic Code:


The Alfven wave-driven wind theory of Hartmann and MacGregor is applied to T Tauri variables, including modifications which permit the calculation of wind temperatures. It is shown that large wave fluxes generate low-temperature winds, which can radiate strongly in Balmer and other optical emission lines. If wave fluxes are restricted to be less than the stellar luminosity, mass loss rates are restricted to values less than or equal to 10 to the -8th solar mass per year. Although these mass loss rates are low in comparison to many previous estimates, it is shown that the wind models produce optical and ultraviolet emission roughly consistent with observations. The theory predicts large wave amplitudes, so that 'turbulent' velocities are generally comparable to, or larger than, local expansion velocities in the optical line-emitting regions, thus making the Sobolev approximation invalid. It is suggested that the discrepancy between the mass loss rates predicted here and previously estimated values is due to the inapplicability of the Sobolev approximation in T Tauri winds.

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