Viscous pulsational instability of the transonic region of isothermal geometrically thin accretion discs. I - Analytical results

Details Viscous pulsational instability of the transonic region of isothermal geometrically thin accretion discs. I - Analytical results Viscous pulsational instability of the transonic region of isothermal geometrically thin accretion discs. I - Analytical results

Mar 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.231...37k&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 231, March 1, 1988, p. 37-48. NASA-supported research.

Statistics

Computation

64

Accretion Disks, Black Holes (Astronomy), Computational Astrophysics, Isothermal Flow, Magnetohydrodynamic Stability, Transonic Flow, Neutron Stars, Perturbation Theory, Radial Flow, Sound Waves, Stellar Oscillations

Scientific paper

Viscous instability of the transonic region of the conventional geometrically thin alpha-type accretion disks is examined analytically. For simplicity, isothermal disks and isothermal perturbations are assumed. It is found that when the value of alpha is larger than a critical value the disk is unstable against two types of perturbations. One is local propagating perturbations of inertial acoustic waves. Results suggest the possibility that unstable perturbations develop to overstable global oscillations which are restricted only in the innermost region of the disk. The other is standing growing perturbations localized just at the transonic point. The cause of these instabilities is that the azimuthal component of the Lagrangian velocity variation associated with the perturbations becomes in phase with the variation of the viscous stress force. Because of this phase matching work is done on perturbations, and they are amplified.

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