Theoretically predicted mass loss rates versus luminosity for different stages in the development of our model atmosphere code. (The mass loss rates were computed using different sets of stellar parameters, but assuming solar metallicity, from:  1990: theoretical evolutionary tracks, cf. Pauldrach et al. 1990;  1996: observationally determined parameters from Puls et al. 1996;  2011 (current version of the code): observationally determined parameters from Repolust et al. 2004.) The solid lines represent simple linear fits to the calculated values. (For the 1996 sample, the five stars with the lowest luminosities have not been included in the fit.)