Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...349..168h&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 349, Jan. 20, 1990, p. 168-189.
Astronomy and Astrophysics
Astrophysics
86
Emission Spectra, Stellar Evolution, Stellar Models, Stellar Winds, T Tauri Stars, Chromosphere, H Alpha Line, Line Spectra, Radiative Transfer, Resonance Lines, Stellar Spectrophotometry
Scientific paper
Line fluxes and profiles are computed for a sequence of spherically symmetric T Tauri wind models. The calculations indicate that the H-alpha emission of T Tauri stars arises in an extended and probably turbulent circumstellar envelope at temperatures above about 8000 K. The models predict that Mg II resonance line emission should be strongly correlated with H-alpha fluxes; observed Mg II/H-alpha ratios are inconsistent with the models unless extinction corrections have been underestimated. The models predict that most of the Ca II resonance line and IR triplet emission arises in dense layers close to the star rather than in the wind. H-alpha emission levels suggest mass loss rates of about 10 to the -8th solar mass/yr for most T Tauri stars, in reasonable agreement with independent analysis of forbidden emission lines. These results should be useful for interpreting observed line profiles in terms of wind densities, temperatures, and velocity fields.
Avrett Eugene H.
Calvet Nuria
Hartmann Lee
Loeser Rudolf
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