Radial self-gravity of accretion disc around supermassive black holes

Details Radial self-gravity of accretion disc around supermassive black holes Radial self-gravity of accretion disc around supermassive black holes

Oct 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ap%26ss.172..293y&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 172, no. 2, Oct. 1990, p. 293-304. Research supported by NNSFC.

Statistics

Computation

3

Accretion Disks, Black Holes (Astronomy), Computational Astrophysics, Gravitational Collapse, Active Galactic Nuclei, Angular Velocity, Quasars, Self Consistent Fields, Viscosity

Scientific paper

The self-gravity characteristics of accretion disks around supermassive black holes are investigated using a global model of self-gravity with thin disk configuration, that includes both the radial and the vertical components. Results show that, for accretion disks around supermassive black holes with M values between 10 to the 8th and 10 to the 10th solar masses, at distances where the R/Rg ratio is about 100,000 to 10,000, the radial component of self-gravity dominates over the central component where the dynamical structure of an accretion disk completely differs from that of Keplerian disk. Results point to the existence of turbulence driven by radial self-gravity instability as a kind of energy source.

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