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We provide global models of line-driven winds of B supergiants formetallicities corresponding to the Large and Small Magellanic Clouds. Thevelocity and density structure of the models is determined consistently fromhydrodynamical equations with radiative force derived in the comoving frame andlevel populations computed from kinetic equilibrium equations. We provide aformula expressing the predicted mass-loss rates in terms of stellarluminosity, effective temperature, and metallicity. Predicted wind mass-lossrates decrease with decreasing metallicity as $\dot M\sim Z^{0.60}$ and areproportional to the stellar luminosity. The mass-loss rates increase below theregion of the bistability jump at about 20\,kK because of iron recombination.In agreement with previous theoretical and observational studies, we find asmooth change of wind properties in the region of the bistability jump. Withdecreasing metallicity, the bistability jump becomes weaker and shifts to lowereffective temperatures. At lower metallicities above the bistability jump, ourpredictions provide similar rates to those used in current evolutionary models,but our rates are significantly lower than older predictions below thebistability jump. Our predicted mass-loss rates agree with observationalestimates derived from H$\alpha$ line assuming that observations of stellarwinds from Galaxy and the Magellanic Clouds are uniformly affected by clumping.The models nicely reproduce the dependence of terminal velocities ontemperature derived from ultraviolet spectroscopy.

New mass-loss rates of Magellanic Cloud B supergiants from global wind models