Mass-loss rates of stars in the Galaxy (left), LMC (middle), and SMC (right) as a function of the Eddington parameter. The discrete symbols indicate stars from different spectral classes. The symbols are color-coded according to a star’s current mass. To enable a comparison to different mass-loss recipes (different rows) that do not have a direct dependence on Γ_e, we calculated stellar evolution models that predict how Γ_e changes during a star’s evolution. Lines indicate how $\dot{M}$ and Γ_e change in the stellar evolution models with initial masses of M_ini = 15 M_⊙ (solid line), 30 M_⊙ (dashed line), 60 M_⊙ (dash-dotted line), and 90 M_⊙ (dotted line) using different mass-loss recipes. The models shown here are calculated until either the surface hydrogen abundance drops below X_H < 0.7 (i.e., when the models would interpolate between MS and WR wind) or until a temperature below T < 12 kK (i.e., when the models would switch to an RSG wind) is reached. Hence, these models should not be compared to the classical WR stars. The different symbols on the lines mark the zero-age main sequence (squares), the terminal-age main sequence (circles), and the aforementioned stopping criterion (diamond).