Notes. The parameters denoted by “CSH” have been taken from Crowther et al. (2010), whereas the parameters of model “A⁻” show our consistently calculated dynamical values for almost the same set of stellar parameters. The result is a too low mass loss rate Ṁ and a too high terminal velocity v_∞ of our model, indicating strongly that the mass M_∗ of the object, which has been assumed by Crowther et al. (2010) on basis of main-sequence evolutionary models (cf. Hirschi et al. 2004), is too high for the given radius (cf. Fig. 22 and Table 13). Scaled solar abundances with the usual scaling factor of 0.5 for the LMC have been adopted for all metals other than those given in the table. (Regarding the values of the solar abundances we refer to Asplund et al. 2009.)