Abstract
A numerical hydrodynamics code is used to investigate two aspects of the winds of hot stars. The first is the question of the instability of the massive radiatively-driven wind of an O star that is caused by the line shape mechanism: modulation of the radiation force by velocity fluctuations. The evolution of this instability is studied in a model O star wind, and is found, modulo some numerical uncertainty, to lead to wave structures that are compatible with observations of wind instabilities. The other area of investigation is of main-sequence B star winds. Attempts were made to simulate a radiatively-driven and a pulsation-driven wind in a B star, but in each case the wind turned out to be very weak. It is argued that the pulsation-driven wind model is not likely to apply to B stars.
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Castor, J.I., Owocki, S.P., Rybicki, G.B. (1988). Time-Dependent Mass Loss from Hot Stars with and without Radiative Driving. In: Stalio, R., Willson, L.A. (eds) Pulsation and Mass Loss in Stars. Astrophysics and Space Science Library, vol 148. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3029-2_14
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DOI: https://doi.org/10.1007/978-94-009-3029-2_14
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