Radiation driven winds of hot luminous stars. IX. Constraints on the wind temperature of O-stars.

The authors present the basic framework of their treatment of theoretical models of radiatively driven winds. The present stage of their wind models, which recently have been extended to include atmospheric models, is described. The calculations, which have been applied on two objects, the O4I(n)f star ζ Pup and the O9.5Ia supergiant α Cam, reveal that only the population of trace ions of low and extremely high stages are affected by the incompleteness of the new models, while the basic ionization structure and hence the wind-dynamics are correct. It is also indicated that for the existence of "superionised" ions the Auger ionisation is possibly of secondary importance in the accelerating part of the wind. The authors conclude that a small amount of non-radiative heating is probably necessary to explain all of the observed O star characteristics.