Upper mass-loss limits and clumping in the intermediate and outer wind regions of OB stars

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Fig. 2

Schematic of the wind emission: different wind regions as a function of the spectral range and their corresponding radial distance to the photosphere (r), as defined in Table 4. The emission model corresponds to the unclumped stellar wind of a O supergiant star (T_eff = 33 kK, Ṁ = 8.6 × 10⁻⁶ M_⊙ yr⁻¹).

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