Chemical abundances of fast-rotating massive stars - I. Description of the methods and individual results

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Fig. E.9

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Same as Fig. E.1, but for HD 46056 (O8Vn; vsin i = 350 km s^-1). While other He lines appear well fitted, He ii 4686 is too weak in the model, which is explained by the fact that wind parameters were not derived (see Sect. 4.3.2).

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