Stability of the Transition Layer between Advection-Dominated and Cooling-Dominated Regions in Accretion Disks. I. Dynamical Instability of Thin Transition

Details Stability of the Transition Layer between Advection-Dominated and Cooling-Dominated Regions in Accretion Disks. I. Dynamical Instability of Thin Transition Stability of the Transition Layer between Advection-Dominated and Cooling-Dominated Regions in Accretion Disks. I. Dynamical Instability of Thin Transition

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999pasj...51...71k&link_type=abstract

Publications of the Astronomical Society of Japan, v.51, p.71-79.

Astronomy and Astrophysics

Astronomy

4

Accretion, Accretion Disks, Advection-Dominated Accretion Flows, Galaxies: Nuclei, Instability: Rayleigh--Taylor Instability, Time Variaions, Transition Region, X-Rays: Sources

Scientific paper

The time variations and Fe fluorescence lines observed in the hard state of stellar black-hole candidates and AGNs might be related to both the instability of and cool gas supply from the transition layer between advection-dominated and cooling-dominated regions. As a first step to examine this possibility, we consider the dynamical instability of the transition layer against non-axisymmetric perturbations under some idealizations. That is, the transition layer is assumed to have an infinitesimal thickness, and perturbations occur inviscidly and adiabatically. No magnetic field is assumed. The results show that the perturbations with mm_crit become overstable due to a density inversion (the Rayleigh--Taylor instability in a rotating system). Here, m_crit ~ 0.085(r/H)2 , r being the radius of the transition region and H the disk half-thickness outside the region. This means that perturbations grow if their size in the azimuthal direction is shorter than ~ 74(H/r)H, which is ~ 2H when H/r=0.03. The limitations of applicability of our results and other possible mechanisms which make the transition layer unstable are discussed in the final section.

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