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Numerical Simulations of Pulsationally Unstable Accretion Disks around Supermassive Black Holes

Published online by Cambridge University Press:  12 April 2016

F. Honma ,
R. Matsumoto  and
S. Kato
F. Honma
Affiliation:
Department of Astronomy, Faculty of Science, Kyoto University, Sakyo-ku, Kyoto 606-01, Japan
R. Matsumoto
Affiliation:
College of Arts and Sciences, Chiba University, Yayoi-cho, Chiba 260
S. Kato
Affiliation:
Department of Astronomy, Faculty of Science, Kyoto University, Sakyo-ku, Kyoto 606-01, Japan

Abstract

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The innermost region of slim accretion disks with standard α viscosity is unstable against axisymmetric radial inertial acoustic perturbations under certain conditions. Numerical simulations are performed in order to demonstrate behaviors of such unstable disks. It is shown that oscillations with the period of ~ 10−3(MBH/M⊙) s can be excited near the inner edge of the disks, where MBH is the mass of the central object. This kind of unstable disks is a possible origin of the periodic X-ray time variabilities with period of ~ 104s observed in a Seyfert galaxy NGC 6814.

Type
III. Models
Information
International Astronomical Union Colloquium , Volume 134: Nonlinear Phenomena in Stellar Variability , 1993 , pp. 365 - 367
Copyright
Copyright © Kluwer 1993

References

Honma, F., Matsumoto, R., and Kato, S: 1992, submitted to Publications of the ASJ Google Scholar
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