Abstract
Some of the fundamental concepts of magnetic rotator theory for stellar winds are reviewed. The distinctions between slow magnetic rotator, fast magnetic rotator and the extreme case of centrifugal magnetic rotator winds are explained. Special emphasis is given to the stellar properties which determine the energy deposition, mass loss rate, and the terminal wind speed. Magnetic rotator winds are always hybrid winds, in which there is a “primary” wind mechanism that determines the mass loss in absence of rotation, and the magnetic rotator forces, which can modify the velocity structure and in the most extreme cases, greatly increase the mass loss rate. Results are presented for the “Luminous Magnetic Rotator ” wind model in which the primary wind mechanism is the line radiation driving force. The results are applied to the hypergiant B[e] and the Wolf Rayet stars; two classes of stars which may have a sequential evolutionary connection. For the Wolf Rayet stars the Luminous Magnetic Rotator model may be able to explain the long standing “wind momentum problem” as well as the “spin-down problem” associated with earlier rotating wind models. Constraints on the surface magnetic field as determined from interior considerations are also discussed.
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