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Nonlinear Phenomena in Stellar Variability pp 83–103Cite as

Accretion Disk Instabilities

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Abstract

Basic properties of accretion disk instabilities are summarized. We first explain the standard disk model by Shakura and Sunyaev. In this model, the dominant sources of viscosity are assumed to be chaotic magnetic fields and turbulence in gas flow, and the magnitude of viscosity is prescribed by so-called α model. It is then possible to build a particular disk model. In the framework of the standard model, accretion disks are stationary, but when some of the basic assumptions are relaxed, various kinds of instabilities appear. In particular, we focus on the thermal limit-cycle instability caused by partial ionization of hydrogen (and helium). We demonstrate that the disk instability model well accounts for the basic observed features of outbursts of dwarf novae and X-ray nova. We then introduce other kinds of instabilities based on the α viscosity model. They are suspected to produce time variabilities observed on a wide range of timescales in close binaries and active galactic nuclei.

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Author information

Authors and Affiliations

  1. Department of Physics, Ibaraki University, Mito 310, Japan

    S. Mineshige

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  1. S. Mineshige
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Editors and Affiliations

  1. Astronomical Institute, Tôhoku University, Sendai, Japan

    M. Takeuti

  2. University of Florida, Gainsville, USA

    J.-R. Buchler

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© 1993 Springer Science+Business Media Dordrecht

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Mineshige, S. (1993). Accretion Disk Instabilities. In: Takeuti, M., Buchler, JR. (eds) Nonlinear Phenomena in Stellar Variability. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-1062-4_8

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  • DOI: https://doi.org/10.1007/978-94-011-1062-4_8

  • Publisher Name: Springer, Dordrecht

  • Print ISBN: 978-94-010-4462-2

  • Online ISBN: 978-94-011-1062-4

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