Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988pmls.conf..229c&link_type=abstract
Pulsation and Mass Loss in Stars, Proceedings of a workshop, held in Trieste, Italy, September 14-18, 1987, Dordrecht: Kluwer, 1
Astronomy and Astrophysics
Astrophysics
1
Cosmic Rays, Hot Stars, Radiation Pressure, Stellar Winds, Losses, Time Dependence, Velocity
Scientific paper
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 is8studied 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.
Castor John I.
Owocki Stanley P.
Rybicki George B.
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