Self-gravitation in spherically symmetric accretion

Details Self-gravitation in spherically symmetric accretion Self-gravitation in spherically symmetric accretion

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.207..861w&link_type=abstract

i, Royal Astronomical Society, Monthly Notices (ISSN 0035-8711), vol. 207, April 15, 1984, p. 861-865.

Astronomy and Astrophysics

Astronomy

4

Accretion Disks, Black Holes (Astronomy), Galactic Nuclei, Gravitational Collapse, Quasars, Galactic Evolution, Gravitational Fields, Interstellar Gas, Luminosity

Scientific paper

The author reconsiders the problem of spherical accretion. He qualitatively treats the aspects of self-gravitation and the increase of the mass of the accreting object due to the accreted matter. It is concluded that when self-gravity is unimportant initially, it cannot become very important. In this case the logarithmic accretion rate m(∝ M/M) has an upper limit, dependent only on the density of the accreted medium. This may imply a luminosity limit lower than the Eddington limit. These results are discussed in the context of an evolutionary picture for quasars as massive black holes accreting from the interstellar gas in galactic cores.

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