Volume 368, Number 1, March II 2001
|Page(s)||311 - 324|
|Section||Atomic, molecular, and nuclear data|
|Published online||15 March 2001|
Entropic-acoustic instability of shocked Bondi accretion I. What does perturbed Bondi accretion sound like?
Service d'Astrophysique, CEA/DSM/DAPNIA, CE-Saclay, 91191 Gif-sur-Yvette, France
Corresponding author: T. Foglizzo, email@example.com
Accepted: 21 December 2000
In the radial flow of gas into a black hole (i.e. Bondi accretion), the infall of any entropy or vorticity perturbation produces acoustic waves propagating outward. The dependence of this acoustic flux on the shape of the perturbation is investigated in detail. This is the key process in the mechanism of the entropic-acoustic instability proposed by Foglizzo & Tagger ([CITE]) to explain the instability of Bondi-Hoyle-Lyttleton accretion. These acoustic waves create new entropy and vorticity perturbations when they reach the shock, thus closing the entropic-acoustic cycle. With an adiabatic index , the linearized equations describing the perturbations of the Bondi flow are studied analytically and solved numerically. The fundamental frequency of this problem is the cut-off frequency of acoustic refraction, below which ingoing acoustic waves are refracted out. This cut-off is significantly smaller than the Keplerian frequency at the sonic radius and depends on the latitudinal number l of the perturbations.When advected adiabatically inward, entropy and vorticity perturbations trigger acoustic waves propagating outward, with an efficiency which is highest for non radial perturbations . The outgoing acoustic flux produced by the advection of vorticity perturbations is always moderate and peaks at rather low frequency. By contrast, the acoustic flux produced by an entropy wave is highest close to the refraction cut-off. It can be very large if γ is close to . These results suggest that the shocked Bondi flow with is strongly unstable with respect to the entropic-acoustic mechanism.
Key words: accretion, accretion disks / hydrodynamics / instabilities / shock waves / binaries: close / X-rays: stars
© ESO, 2001
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