Comparison between the final models and the ones computed using the hydrodynamical mass-loss rates of Vink et al. (2000) in the UV region. The IUE spectra are in solid black, and the star name is indicated right below its spectrum. All the final models (Ṁ from the UV) are in red, while Ṁ_Vink is in dashed black. Our final models have clumping (f_∞ = 0.1), while the models with Ṁ_Vink are unclumped. We note how Ṁ_Vink overestimates the intensity in Si IV λλ1394,1403 for all our sample. C IV lines also become saturated in a few cases, in contrast to the observations.