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Fig. 2


Predicted dependence of the mass-loss rate on luminosity Eq. (1) (solid line) for LMC (upper panel) and SMC (lower panel) in comparison with data derived from optical spectroscopy (red symbols, Massey et al. 2004, 2005; Mokiem et al. 2006, 2007a; Bestenlehner et al. 2014; Ramírez-Agudelo et al. 2017; Sabín-Sanjulián et al. 2017) and UV spectroscopy (violet symbols, Bouret et al. 2003, 2013, 2015). Vertical arrows denote upper limits. The results of Bouret et al. (2015) were derived for stars from IC 1613 and WLM dwarf galaxies, which have a similar metallicity as SMC. Dashed lines denote predictions of Vink et al. (2001) for giants from Table 1.

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