New Insights into Radiation Line-Driven Winds

CIDALE, L.; HAUCKE, M.; CURÉ, M.; VENERO, R.

Praga

Congreso; The B[e] Phenomenon: Forty Years of Studies; 2016

IAU

The classical theory of radiatively driven stellar winds reproduces the observedstellar wind conditions (mass loss and terminal velocity) of massive supergiantsfairly well. However, some differences are still found between the wind parameters predicted by theory and those observed in mid-B, late-B, and A-type supergiants. Inclusion of rotation in the models brought a remarkable progress in the development of the theory of stellar winds. Three types of stationary wind regimes are currently known: the classical fast solution, the Ω− slow solution that arises for fast rotators, and the δ− slow solution that takes place in highly ionized winds. We show synthetic line profiles and discuss all the hydrodynamical solutions in the context of the observed wind properties of B and B[e] supergiants. We also discuss the variability of spectral lines formed in the wind of B-supergiants.