Non-axisymmetric hydrodynamic instability and transition to turbulence in two-dimensional accretion discs.

Details Non-axisymmetric hydrodynamic instability and transition to turbulence in two-dimensional accretion discs. Non-axisymmetric hydrodynamic instability and transition to turbulence in two-dimensional accretion discs.

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999phr...311..271g&link_type=abstract

Physics Reports, Vol. 311, No. 3 - 5, p. 271 - 278

Physics

1

Accretion Disks: Instabilities, Accretion Disks: Turbulence, Oscillations: Dwarf Novae

Scientific paper

The non-linear growth of a non-axisymmetric instability in geometrically thin Keplerian discs is followed numerically with the use of a time-dependent two-dimensional polytropic hybrid Fourier-Chebyshev spectral method of collocation. The non-axisymmetric instability (a corotation resonance) develops in the inner disc when the inner boundary is rigid (corresponding here to the surface of an accreting compact star). When the viscosity is low, the high-order modes dominate the flow. It is found, for α = 0.001, that the flow undergoes a subcritical transition to turbulence. The turbulence is confined in the inner region of the disc, inside the 'resonant cavity', where it sustains itself in the same manner as the non-axisymmetric instability itself. Due to the inverse cascade of energy characteristic of two-dimensional flow, the m = 1 mode eventually dominates. The turbulence obtained in this work cannot account for angular momentum transport in the disc. However, the instability provides a new robust mechanism to explain the appearance of short-period oscillations (dwarf nova oscillations and quasiperiodic oscillations) observed in the inner disc of cataclysmic variables and other systems.

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