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We have calculated a grid of massive star wind models and mass-loss rates fora wide range of metal abundances between 1/100 and 10 Z/Zsun.  The calculation of this grid completes the Vink et al. (2000) mass-lossrecipe with an additional parameter Z. We have found that the exponent of thepower law dependence of mass loss vs. metallicity is constant in the rangebetween 1/30 and 3 Z/Zsun. The mass-loss rate scales as Mdot \propto Z^0.85Vinf^p with p = -1.23 for stars with Teff \ga 25000 K, and p = -1.60 for the Bsupergiants with Teff \la 25000 K. Taking also into account the metallicitydependence of Vinf, using the power law dependence Vinf \propto Z^0.13 fromLeitherer et al. (1992), the overall result of mass loss as a function ofmetallicity can be represented by Mdot \propto Z^0.69 for stars with Teff \ga25000 K, and Mdot \propto Z^0.64 for B supergiants with Teff \la 25000 K.  Our mass-loss predictions are successful in explaining the observed mass-lossrates for Galactic and Small Magellanic Cloud O-type stars, as well as inpredicting the observed Galactic bi-stability jump. Hence, we believe that ourpredictions are reliable and suggest that our mass-loss recipe be used infuture evolutionary calculations of massive stars at different metal abundance.A computer routine to calculate mass loss is publicly available.Comment: Accepted by A&A, 16 pages, (email: jvink@ic.ac.uk

Mass-loss predictions for O and B stars as a function of metallicity