New predictions for radiation-driven, steady-state mass-loss and wind-momentum from hot, massive stars - II. A grid of O-type stars in the Galaxy and the Magellanic Clouds

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Fig. 4

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Converged velocity structure for the characteristic model of Sect. 2.2, showing velocity over terminal wind speed versus the scaled radius-coordinate in black. The green line shows a fit using a double β-law following Eq. (22) (see text for details).

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