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Resonance Line Profiles from Radial Accretion Flows

  • R. Tylenda
Conference paper
Part of the Astrophysics and Space Science Library book series (ASSL, volume 145)

Abstract

A compact star in a detached binary system can accrete the matter from the stellar wind of the companion. In this case a more or less radial accretion flow is formed. By analogy to stellar winds from early type stars it is usually believed that the accretion of this sort should produce inverse P-Cygni profiles in resonance lines. However, there are physical differences between the wind and the radial accretion which can alter the outgoing profile significantly.

Keywords

Line Profile Optical Thickness Resonance Line Stellar Wind Compact Star 
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.

References

  1. Natta, A., Beckwith, S., 1986, Astron. Astrophys. 158, 310.ADSGoogle Scholar

Copyright information

© Kluwer Academic Publishers 1988

Authors and Affiliations

  • R. Tylenda
    • 1
  1. 1.Laboratory for AstrophysicsCopernicus Astronomical CentreTorunPoland

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