Hostname: page-component-788cddb947-wgjn4 Total loading time: 0 Render date: 2024-10-13T16:53:39.271Z Has data issue: false hasContentIssue false
  • English
  • Français

SPH Simulations of Tidally Unstable Accretion Disks

Published online by Cambridge University Press:  12 April 2016

James Murray
James Murray*
Affiliation:
Canadian Institute for Theoretical Astrophysics, University of Toronto, Ontario M5S 1A7, Canada, jmurray@cita.utoronto.ca

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We use two dimensional Smoothed Particle Hydrodynamics simulations to investigate the the Tidal Resonance Instability (TRI) model for superhumps in SU UMa stars.

In the TRI model, superhumps are the signature of an eccentric disk being periodically stressed by the binary system’s rotating tidal field. A slow prograde motion of the disk in the inertial frame is then responsible for the superhump period slightly exceeding the binary orbital period. The disk eccentricity is caused by a 3:1 resonance between orbits in the disk and the orbit of the binary itself. The development of the TRI model is due mainly to Whitehurst (1988), Hirose & Osaki (1990) and Lubow (1991a). Lubow in particular carried out a nonlinear mode analysis of a fluid disk’s response to a weak tidal field and identified the feedback mechanism responsible for disk eccentricity growth.

Type
Accretion Discs
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 115 - 116
Copyright
Copyright © Kluwer 1996

References

Hirose, M., Osaki, Y., 1990, PASJ, 42, 135 Google Scholar
Lubow, S.H., 1991a, Ap. J., 381, 259 CrossRefGoogle Scholar
Lubow, S.H., 1991b, Ap. J., 381, 268 CrossRefGoogle Scholar
Lubow, S.H., 1992, Ap. J., 401, 317 CrossRefGoogle Scholar
Monaghan, J.J., 1992, ARAA, 30, 543 CrossRefGoogle Scholar
Murray, J.R., 1996, MNRAS, in pressGoogle Scholar
Whitehurst, R., 1988, MNRAS, 232, 35 CrossRefGoogle Scholar