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Fig. 1

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UV spectra for a selection of stars for each spectral type presented in this study, from earlier to later spectral types. Observations (black lines) are shown with best-fit model spectra (red lines). The observational sequence is very nicely reproduced by the models (Table 2). Note the strong transition in wind profiles (e.g. C ivλλ1548, 1550) around spectral type O6 V.

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