All Tables

Table 1: Summary of the extended model atom. The iron-group ions (Fe) are described by a relatively small number of super-levels, each representing a large number of true atomic energy levels (sub-levels). In the present work we also apply a smaller model atom, where the iron-group ions are restricted to Fe II-Fe X with Fe X represented by one auxiliary level.
Table 2: Model parameters for our different test models (A, B, C, and D) and the hydrodynamic model (Hydro) compared to the values derived for WR 111 by (Gräfener et al. 2002). Stellar core parameters: Stellar luminosity $L_\star$ , radius $R_\star$ , temperature $T_\star$ , and mass $M_\star$ (relevant only for the hydrodynamic model). Wind parameters: mass-loss rate $\dot{M}$ with the corresponding transformed radius $R_{\rm t}$ , clumping factor D, and terminal wind velocity $\mbox{$\varv$ }_\infty$ . Atmospheric abundances: mass fractions of helium, carbon, oxygen, silicon and iron $X_{\rm He}$ , $X_{\rm C}$ , $X_{\rm O}$ , $X_{\rm Si}$ , and $X_{\rm Fe}$ . Wind efficiency: resultant work-ratio $Q=W_{\rm wind}/L_{\rm wind}$ according to Eqs. (1) and (2), and wind momentum efficiency $\eta = L_\star / c\dot{M} \mbox{$\mbox{$\varv$ }_\infty$ }$ .