Radiation-driven winds of hot luminous stars XVI. Expanding atmospheres of massive and very massive stars and the evolution of dense stellar clusters

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Fig. 21

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Predicted mass loss rates for the same objects as in Fig. 19 versus Γ, the ratio of stellar luminosity to Eddington luminosity. The curves represent the mass loss rates according to the approximative formula of Eq. (6) for various stellar masses as labelled.

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