Thermal instability of disk accretion by a black hole

Details Thermal instability of disk accretion by a black hole Thermal instability of disk accretion by a black hole

Aug 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975sval....1..158s&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 1, Aug. 1975, p. 6-11.) Soviet Astronomy Letters, vol. 1, July-Aug. 1975, p. 158-160. T

Astronomy and Astrophysics

Astronomy

7

Black Holes (Astronomy), Gravitational Collapse, Thermal Instability, Astronomical Models, Binary Stars, Emission Spectra, Viscosity

Scientific paper

Accretion onto black holes with considerable angular momentum is accompanied by the formation of a disk of accreting material. Disks must form both around black holes of stellar origin in binary systems and around supermassive black holes in the nuclei of galaxies and in quasars. Mass, accretion rate, viscosity, turbulence, disk stability, and the (turbulent pulsation rate)/(sound speed) ratio are analyzed. Accretion is unstable against small perturbations in the inner region of the accretion disk where radiative pressure dominates, and stationary accretion can occur only at a specified value of viscosity.

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