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Studies in Flickering

  • W. F. Welsh
  • Janet H. Wood
  • K. Horne
Part of the Astrophysics and Space Science Library book series (ASSL, volume 208)

Abstract

Flickering is a poorly understood phenomenon associated with accretion processes, but this does not suffice to make it interesting. Why then should we bother studying this ‘noise’? Three reasons come to mind: (i) flickering is a fundamental signature of accretion, to the point of being a necessary characteristic (if it doesn’t flicker, it’s not a CV); (ii) energetically, flickering is not a small effect and can contribute up to a few tens of percent of the total luminosity of the system (hence it is often more luminous than the entire secondary star); (iii) flickering is inherently a time—dependent phenomenon and it is hoped that it can provide clues to the nature of the disc viscosity, something that time—independent theory cannot provide.

Keywords

Light Curve Accretion Disc Light Curf White Dwarf Orbital Phase 
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. 1.
    Bennie, P.J., Hilditch, R.W., Horne, K., 1996, these proceedings, p33Google Scholar
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    Bruch, A., 1996, these proceedings, p35Google Scholar
  3. 3.
    Horne, K., 1985, MNRAS, 213, 129ADSGoogle Scholar
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    Horne, K., Stiening, R.F., 1985, MNRAS, 216, 933ADSGoogle Scholar
  5. 5.
    Welsh, W.F., Wood, J.H., 1995, in “Flares & Flashes” — Proc. of IAU Colloquium 151, eds. J. Greiner, H.W. Duerbeck, R.E. Gershberg, Springer-Verlag, p300Google Scholar

Copyright information

© Kluwer Academic Publishers 1996

Authors and Affiliations

  • W. F. Welsh
    • 1
  • Janet H. Wood
    • 1
  • K. Horne
    • 2
  1. 1.Keele UniversityUK
  2. 2.University of St. AndrewsUK

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