Abstract
We present a quantitative study of the variability in ultraviolet resonance lines of N v, Si Iv and C Iv of the Be star γ Cas, following up on the work of Henrichs et al. (1983). For this purpose we used 133 IUE spectra obtained over a period of eleven years. Variability occurs in the form of discrete absorption components (DACs), which are formed in the fast-outflowing radiatively driven part of the stellar wind. We constructed a template spectrum from spectra containing no or minor extra absorption due to DACs and modelled the isolated DACs in the obtained quotient spectra. Besides the frequently observed narrow components (u t typically ≤ 250 km/s) at high velocity, we found several broad components occurring at low and intermediate wind velocities.
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