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Time-Dependent Mass Loss from Hot Stars with and without Radiative Driving

  • John I. Castor
  • Stanley P. Owocki
  • George B. Rybicki
Conference paper
Part of the Astrophysics and Space Science Library book series (ASSL, volume 148)

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.

Keywords

Radiation Force Column Density Absorption Approximation Reverse Shock Narrow Component 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Kluwer Academic Publishers 1988

Authors and Affiliations

  • John I. Castor
    • 1
  • Stanley P. Owocki
    • 2
  • George B. Rybicki
    • 3
  1. 1.Lawrence Livermore National LaboratoryUSA
  2. 2.Bartol Research InstituteUSA
  3. 3.Harvard-Smithsonian Center for AstrophysicsUSA

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