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Comoving frame calculations for λ-cephei

  • Nadine Rons
  • Mark Runacres
  • Ronny Blomme
III. Stellar Winds and Massive Stars
Part of the Lecture Notes in Physics book series (LNP, volume 401)

Abstract

Many stars continuously eject material and thus surround themselves with a stellar wind. We can observe this wind indirectly through its characteristic effects on the stellar spectrum. In particular, this mass flow influences the line profiles. These so called P-Cygni profiles can be observed in the visual part of the spectrum of early-type stars and Wolf-Rayet stars, as well as - and even more clearly - in the ultraviolet part. In order to study the stellar wind structure, a computer programme was written which calculates theoretical P-Cygni profiles using the Comoving Frame Method. As input, this code can use the results obtained from other programmes, such as a non-LTE code. Through parameter adjustments a fit to an observed profile can be made.

Keywords

Optical Depth Source Function Stellar Wind Visual Part Stellar Surface 
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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References

  1. Groenewegen, M.A.T., Lamers, H.J.G.L.M., 1989, Astron. Astrophys. Suppl. Ser. 79, 359.Google Scholar
  2. Mihalas, D., Kunasz, P.B., Hummer, D.G., 1975, Astrophys. J. 202, 465.Google Scholar

Copyright information

© Springer-Verlag 1992

Authors and Affiliations

  • Nadine Rons
    • 1
  • Mark Runacres
    • 1
  • Ronny Blomme
    • 2
  1. 1.Astrofysisch InstituutVrije Universiteit BrusselBrusselBelgium
  2. 2.Koninklijke Sterrenwacht BelgiëBrusselBelgium

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