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Massive stars lose a large fraction of their mass to radiation-driven windsthroughout their entire life. These outflows impact both the life and death ofthese stars and their surroundings. Theoretical mass-loss rates of hot, massivestars are derived to be used in applications such as stellar evolution. Thebehaviour of these rates in the OB-star regime is analysed, and their effectson massive-star evolution predictions is studied. Dynamically-consistent modelsare computed by solving the spherically symmetric, steady-stateequation-of-motion for a large grid of hot, massive stars. The radiativeacceleration is derived from non-local thermodynamic equilibrium radiativetransfer in the co-moving frame. The resulting mass-loss rates are used toderive a simple scaling recipe with stellar parameters and to evaluate somefirst impacts upon evolution tracks. We provide a new prescription forsteady-state, radiation-driven mass-loss from hot, massive stars depending ontheir fundamental parameters. The rates for O-stars are lower by about a factor~3 than the rates typically used in previous stellar-evolution calculations,where differences generally decrease with increasing luminosity andtemperature. For cooler B-giants/supergiants we find larger discrepancies. Thisarises because we do not find any systematic increase in mass-loss rates belowthe so-called bi-stability region; indeed, our results do not show any sign ofa significant bi-stability jump within the parameter range covered by the grid.Due to the lower mass-loss rates we find that envelopes are not easily strippedby means of standard steady-state winds, making it difficult to createclassical Wolf-Rayet stars via this channel. However, a remaining keyuncertainty regarding these predictions concerns unsteady mass loss for veryhigh-luminosity stars close to the Eddington limit as well as the impact ofnon-line-driven winds.

New predictions for radiation-driven, steady-state mass-loss and  wind-momentum from hot, massive stars III. Updated mass-loss rates for  stellar evolution