Time-dependent mass loss from hot stars with and without radiative driving
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, /ital 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. 28 refs., 11 figs.
- Research Organization:
- Lawrence Livermore National Lab., CA (USA); Bartol Research Foundation of the Franklin Inst., Newark, DE (USA); Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (USA)
- DOE Contract Number:
- W-7405-ENG-48
- OSTI ID:
- 5099637
- Report Number(s):
- UCRL-98097; CONF-8709261-1; ON: DE88008899
- Resource Relation:
- Conference: Trieste workshop on pulsation and mass loss in stars, Trieste, Italy, 14 Sep 1987
- Country of Publication:
- United States
- Language:
- English
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