A runaway instability in thick accretion disks?

Details A runaway instability in thick accretion disks? A runaway instability in thick accretion disks?

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984natur.312..620w&link_type=abstract

Nature (ISSN 0028-0836), vol. 312, Dec. 13, 1984, p. 620, 621. Research supported by the Science and Engineering Research Counci

Astronomy and Astrophysics

Astrophysics

25

Accretion Disks, Astrophysics, Black Holes (Astronomy), Stellar Mass Accretion, Dynamic Stability, Energy Transfer, Relativistic Effects

Scientific paper

It has been proposed that thick disks of material accreting around black holes may be subject to a runaway instability. If the mass of the disk exceeds a critical value (mdisk > 0.01 Mhole), the disk drains into the hole on a dynamical time scale. The author reports a study of this effect, using models of non-self-gravitating disks in the Kerr metric, which enables proper allowance to be made for the effects of black-hole rotation and the increase in the spin of the hole as it accretes. It is concluded that there is no runaway instability in these systems.

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