Hydrodynamic Simulation of Accretion Disks in Cataclysmic Variables

  • M. Hirose
  • Yoji Osaki
Part of the NATO ASI Series book series (ASIC, volume 290)

Abstract

The non-axisymmetric configurations of accretion disks in cataclysmic variables are studied by two-dimensional hydrodynamical calculations. The particle-hydrodynamic method first developed by Lin and Pringle (1976) is used, and time evolution of accretion disks under a constant mass supply rate from the secondary is followed until the system settles to a quasi-steady state. It is found that a binary system with comparable masses of component stars settles to a steady state of an elongated disk fixed in the rotating frame of the binary while in the case of low mass secondary it settles to a periodic oscillating state in which a non-axisymmetric (eccentric) structure is formed and it rotates slowly in the inertial frame of reference. The period of oscillation is a few percent longer than the orbital period of binary, and it offers a natural explanation to the “superhump” periodicity of SU UMa stars. Our results thus confirm basically those of Whitehurst (1988) who has discovered the tidal instability of an accretion disk in a low mass secondary.

Keywords

Orbital Period Light Curve Accretion Disk Roche Lobe Hydrodynamic Simulation 
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. Lin, D.N.C. and Pringle, J.E., 1976, IA U Symp. No. 73, p237, eds Eggleton, P., Mitton, S., and Whelan, J., Reidel, Dordrecht, HollandGoogle Scholar
  2. Paczynski, B. 1977, Astrophys. J., 216, 822ADSCrossRefGoogle Scholar
  3. Whitehurst, R. 1988, Monthly Notices Roy. Astron. Soc., 232, 35ADSGoogle Scholar

Copyright information

© Kluwer Academic Publishers 1989

Authors and Affiliations

  • M. Hirose
    • 1
  • Yoji Osaki
    • 1
  1. 1.Department of Astronomy, Faculty of ScienceUniversity of TokyoBunkyo-kuJapan

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