Top: global line profile (i.e. combining the Be-disc and photo-spheric contributions and accounting for the full array of transitions) for our default magnetic interaction model, at two opposite quadrature orbital phases. The profiles are shown as histograms binned in energy bins of 1 eV. Bottom: convolution of the global line profiles with an instrumental response function of 5 eV FWHM. The magenta lines yield the theoretical energies of the centroids of the Fe V Kα1 and Kα2 subgroups (Palmeri et al. 2003) assuming Fe IV target ions.