Fig. 2
Mass-luminosity relation for WR stars without hydrogen (in black) compared to the limits given by Eq. (8) for the same composition and various Γ-values as indicated. The continuous black line refers to models by Gräfener et al. (2011) with X = 0, while the broken black line represents the average mass-luminosity of WR stars without hydrogen from Schaerer & Maeder (1992).
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