Abstract
The resonance spectral lines of high-resolution IUE spectra of χ2 Ori (B2I) have been studied with the aim to determine in more detail the physical status of the stellar wind and its variability due to shell outbursts and clumps superimposed on the isotropic stellar wind. Some general features of resonance spectral line profiles have been studied and explained in physical terms using χ2 Ori as a specimen.
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