Abstract
The radiatively driven wind theory does not correctly predict the observed values of the terminal velocity and mass loss rate for O and early B-type stars. Hoping to explain this discrepancy the authors investigated how sensitive the theoretical predictions are to errors in the oscillator strengths. The results show that the stellar wind dynamics is quite sensitive to changes in the oscillator strengths for the iron-group elements. For some stars the mass loss rate increases by a factor of 2, bringing them much closer to the observed rates. Unfortunately at the same time the terminal velocity also increases, making the discrepancy of that parameter with the observations even larger.
