Stellar mass-loss near the Eddington limit - Tracing the sub-photospheric layers of classical Wolf-Rayet stars

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Fig. 12

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Comparison of envelope solutions in the mass range from 8 M_⊙ (bottom) to 23.7 M_⊙ (top) with the semi-empirical sonic-point conditions from Sect. 4.2 (black dots). The thick black curve indicates our previous example model with 14 M_⊙, and the grey dashed line the wind condition Eq. (23).

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