WR Wind Models: [WC]-Type CSPN vs. Massive Stars
G. Gräfener, W.-R. Hamann, H. Todt
The optically thick stellar winds of Wolf-Rayet (WR) stars have recently been explained by means of hydrodynamic model atmospheres. In the present talk we discuss the physical processes that lead to their formation for the case of young massive stars as well as for [WC]-type CSPN. We explain why we expect WR-type mass loss only in specific temperature regimes, and discuss the possibility of pulsational wind driving for other cases.
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