Hydrodynamic instability of accretion flows and wind flows with standing shock waves

Details Hydrodynamic instability of accretion flows and wind flows with standing shock waves Hydrodynamic instability of accretion flows and wind flows with standing shock waves

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.259..259n&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 259, no. 2, p. 259-264.

Statistics

Computation

18

Black Holes (Astronomy), Flow Stability, Shock Waves, Stellar Mass Accretion, Stellar Winds, Accretion Disks, Computational Fluid Dynamics, Standing Waves

Scientific paper

The hydrodynamic instability of isothermal, inviscid and axisymmetric accretion (and wind) flows with standing shock waves is studied against infinitesimal, isothermal, and axisymmetric perturbations. The post-shock flow is assumed to be transonic so that accretion on to black holes can be treated. A global stability analysis shows that the value of an unperturbed quantity, nu is identical to (1/V)(d-Phi-eff/dr-cs-squared/r), at the post-shock side of the unperturbed shock location determines stability properties, where V, Cs, and Phi-eff are, respectively, the radial flow velocity, the isothermal sound speed, and effective gravitational potential including the centrifugal force. If nu is not less than 0 no unstable mode exists, in other words nu is less than 0 is a necessary condition for axisymmetric instability. This criterion means that the flow may be unstable only when the fluid decelerates on the pre-shock side. It is found that the growth rates and frequencies of unstable modes are bounded by the absolute value of nu.

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