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Stellar evolution models of massive stars are very sensitive to the adoptedmass-loss scheme. The magnitude and evolution of mass-loss rates significantlyaffect the main sequence evolution, and the properties of post-main sequenceobjects, including their rotational velocities. Driven by potentialdiscrepancies between theoretically predicted and observationally derivedmass-loss rates in the OB star range, we particularly aim to investigate theresponse to mass-loss rates that are lower than currently adopted, in parallelwith the mass-loss behavior at the "first" bi-stability jump. We perform 1Dhydrodynamical model calculations of single $20 - 60 \, M_{\odot}$ Galactic ($Z= 0.014$) stars where the effects of stellar winds are already significantduring the main sequence phase. We develop an experimental wind routine toexamine the behavior and response of the models under the influence ofdifferent mass-loss rates. This observationally guided, simple and flexiblewind routine is not a new mass-loss description but a useful tool based on theWind-momentum Luminosity Relation and other scaling relations, and provides ameaningful base for various tests and comparisons. The main result of thisstudy indicates a dichotomy when accounting for currently debated problemsregarding mass-loss rates of hot massive stars. In a fully diffusive approach,and for commonly adopted initial rotational velocities, lower mass-loss ratesthan theoretically predicted require to invoke an additional source of angularmomentum loss (either due to bi-stability braking, or yet unidentified) tobrake down surface rotational velocities. [...]

Modeling the early evolution of massive OB stars with an experimental wind routine