Abstract
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 & Jefferies in 1990 for static, inhomogeneous media. Both the wind structure (i.e., the velocity, size, and filling factor of the clumps which form the wind) and the gas radiative properties (i.e., optical depth and source function at each distance from the star) 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 Hα in T Tauri stars, and their dependence on the wind parameters
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