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Radiatively driven winds of OB stars

Published online by Cambridge University Press:  26 May 2016

Michihiro R. Shimada ,
Masaki Ito ,
Ryuko Hirata  and
Toshihiro Horaguchi
Michihiro R. Shimada
Affiliation:
Department of Astronomy, Kyoto University, Sakyo-ku, Kyoto, 606-01, Japan
Masaki Ito
Affiliation:
Department of Astronomy, Kyoto University, Sakyo-ku, Kyoto, 606-01, Japan
Ryuko Hirata
Affiliation:
Department of Astronomy, Kyoto University, Sakyo-ku, Kyoto, 606-01, Japan
Toshihiro Horaguchi
Affiliation:
National Science Museum, Ueno Park, Taito-ku, Tokyo 110, Japan

Abstract

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We newly calculated the line radiative force with 520,000 atomic lines, which is twice as many as those of Abbott (1982), for OB supergiants. Our results are as follows. (1) The mass loss rates for O stars with Teff = 50,000K are seven times as large as Abbott's (1982) because of contribution from Fe iv lines. (2) Contribution from many weak lines increases the mass loss rates and decreases the wind velocities of OB stars within a temperature range of 10,000K ≤ Teff ≤ 30,000K. This result is qualitatively in accordance with the results from the recent observations of O stars. (3) The mass loss rates of OB stars depend on metallicity with Ṁ ∼ Z.

Type
7. OB Stellar Winds
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 487 - 489
Copyright
Copyright © Kluwer 1994 

References

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