Non-Axisymmetric Shear Instabilities in Thick Accretion Disks

  • Ramesh Narayan
  • Jeremy Goodman
Part of the NATO ASI Series book series (ASIC, volume 290)


Recent results on the Papaloizou-Pringle non-axisymmetric instability in thick accretion disks is reviewed. Considerable work has been done on “slender” tori and annuli; these are systems whose radial widths are small compared to their mean radii. The linear instabilities in slender configurations fall into two classes, (i) the principal branch, and (ii) higher-order modes. The physical mechanism by which these modes become unstable has been identified. The idealized slender models have been extended in several ways; some work has been reported on (i) modes in wide tori/annuli, (ii) nonlinear development of unstable modes, (iii) role of accretion, (iv) effect of self-gravity, and (v) effect of entropy gradient. These studies have brought us closer to the point where we can tell whether or not the PP instability is important for thick disks in nature. This issue is expected to be resolved by three-dimensional hydrodynamic simulations.


Accretion Disk Unstable Mode Global Mode Thick Disk Principal Mode 
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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Copyright information

© Kluwer Academic Publishers 1989

Authors and Affiliations

  • Ramesh Narayan
    • 1
  • Jeremy Goodman
    • 2
  1. 1.Steward ObservatoryUniversity of ArizonaTucsonUSA
  2. 2.Department of Astrophysical SciencesPrinceton UniversityPrincetonUSA

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