Physics
Scientific paper
Nov 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...489..804m&link_type=abstract
Astrophysical Journal v.489, p.804
Physics
8
Accretion, Accretion Disks, Black Hole Physics, Hydrodynamics, Instabilities, Methods: Numerical
Scientific paper
Runaway instability of accretion disks around black holes, i.e., unstable mass overflow from disks to black holes, has been investigated by computing the time evolution of self-gravitating disks. It is crucial to include self-gravity of the disk in numerical simulations because it has been shown that self-gravity of the disk is the main cause of the instability. Dynamical evolutions of self-gravitating disks with several representative rotation laws, i.e., constant specific angular momentum disks, Kepler-type disks, and constant linear velocity disks, have been pursued by using the smoothed particle hydrodynamics code with 12,000 pseudo-particles. We have found that if the ratio of the disk mass to the black hole mass exceeds about 10-1.8, self-gravitating disks suffer from runaway instability and that the matter of the disks flows down to the central black hole in 1-2 times the dynamical timescale. This is common to almost all models irrespective of rotation laws.
Eriguchi Yoshiharu
Masuda Nobuyuki
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