Notes.The first two rows represent the adopted photospheric parameters, similar to those derived by Najarro et al. (2011) and Bouret et al. (2012). Y_He = N_He∕N_H is the Helium abundance by number, whereas is the mass fraction of element A, normalized to the corresponding abundance from Asplund et al. (2005), and taken from Cohen et al. (2010) (but see text). The following rows (left part) display the wind parameters (for a wind adopted as smooth), with β the exponent of the typical wind velocity law. The right part displays the X-ray emission parameters (cf. Carneiro et al. 2016 for details) common to all models, with maximum shock temperature reached far out in the wind. is the jump velocity, u_j(r), at large distances from the star, where the latter has been parameterized following , with exponent γ_x (see also Pauldrach et al. 1994). We note that .