Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...404..751m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 404, no. 2, p. 751-764.
Astronomy and Astrophysics
Astrophysics
32
Line Spectra, Stellar Models, Stellar Winds, T Tauri Stars, Radiative Transfer, Stochastic Processes
Scientific paper
This paper discusses the formation of spectral lines in stochastic moving media. The method used to solve the radiation transfer is based on that developed by Lindsey and Jefferies (1990) for static, inhomogeneous media. Both the wind structure and the gas radiative properties are considered as free parameters. Most of the calculations are intended to investigate the formation of double-peaked line profiles, as those often seen in H-alpha in T Tauri stars, and their dependence on the wind parameters. Within the limits set by the adopted parametric description of the wind properties, we find that the observed features can be understood if the winds are clumpy and decelerate at large distance from the star. By comparing the model calculations to several observed H-alpha spectra, we assign a typical clump size near the stellar surface of less than about 0.1 stellar radii, and a volume filling factor of about 0.1. From the depth of the absorption dip, there is an indication that the wind remains clumpy also at large distances from the star. Some results for lines of intermediate optical depth are also discussed. We find that in this case the profiles are similar to those obtained in continuous winds of much lower optical depth. In stochastic winds, it is therefore possible to have lines, which while forming in an optically thick gas, have profiles typical of optically thin conditions. This fact can explain the properties of the Ca II infrared triplet lines in many T Tauri stars.
Grinin V. P.
Mitskevich A. S.
Natta Antonella
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