al. (2003) which suggest that the massive winds in LMC O stars recombine at large radius. Stars with massive enough winds to have P [v]{} at low to intermediate velocity, recombine to P [iv]{} at high velocity, thus we do not see the NACs. Inspection of the O supergiant (P[v]{}) sample suggests however that several of the Si [iv]{} profiles in these stars do have NACs. For stars in this sample with well-developed NACs that clearly contrast against the ’underlying’ P Cygni absorption, it would be worthwhile to derive $q($Si$^{3+}$) values for the blue Si[iv]{} NAC since we have demonstrated here that the contrast between from NACs and from intermediate velocity can be of order 3 to 10. A corresponding upward adjustment of the P [v]{} estimates would then place these values closer to the H$\alpha$ estimates and the theoretical predictions.

However, when addressing all of these issues in hot star winds, one must keep in mind that geometry matters. Although some progress has been made modelling the effects that of randomly distributed clumps of various shapes have on wind lines, there is compelling evidence (e.g. Kaper et al. 1996; Fullerton et al. 1997; Prinja et al. 2002) that the 