A local instability of tidally distorted accretion disks

Details A local instability of tidally distorted accretion disks A local instability of tidally distorted accretion disks

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...406..596g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 406, no. 2, p. 596-613.

Physics

54

Accretion Disks, Angular Momentum, Binary Stars, Flow Stability, Gravitational Effects, Stellar Physics, Hydrodynamics, Incompressible Flow, Momentum Transfer, Stellar Gravitation, Turbulence

Scientific paper

Hydrodynamic accretion disks in binary star systems have local, three-dimensional, approximately incompressible instabilities whose growth rate is linearly proportional to the tidal field of the secondary star. The instability occurs throughout the disk but is most rapid in the outer parts. The free energy for the instability derives from the tidal distortion of the disk rather than its differential rotation. The instability will excite m-parallel 1 internal waves of the type discussed by Vishniac et al. (1992), and it should facilitate return of angular momentum from the disk to the secondary star. It is closely related to a recently discovered instability that has been suggested as a mechanism for transition to turbulence in terrestrial and laboratory flows, but whether it will lead to strong turbulence in disks is as yet unclear.

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