The structure and evolution of nuclear discs

Details The structure and evolution of nuclear discs The structure and evolution of nuclear discs

Jul 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982mnras.200..247b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 200, July 1982, p. 247-262. Research supported by the Science and Engin

Astronomy and Astrophysics

Astronomy

15

Astronomical Models, Galactic Evolution, Galactic Nuclei, Interstellar Gas, Stellar Evolution, Stellar Mass Ejection, Black Holes (Astronomy), Density Distribution, Galactic Rotation, Galactic Structure

Scientific paper

An investigation of dense, cold nuclear gas disk evolution as a function of spherical galaxy parameters shows in all cases that the disk growth, which is dominated by infall, continues until the onset of local gravitational instability close to the center in a region where mean mass density is less than 10,000-100,000 solar masses/cu pc. Massive star formation can then propagate sequentially through the disk, leading to a burst of star formation. The theory imposes constraints on both the black hole and spinar models of nuclear activity. In the case of the black hole model, comparison with observations of galactic nuclei shows that there can be little or no correlation between the mass of the hole and the luminosity of its accretion disk, and that the hole must accrete a very small fraction of the available fuel. Spinar model energy generation efficiency is significantly smaller, so that a larger proportion of the fuel must be consumed by recurrent bursts of nuclear activity which individually terminate in the explosive disruption of the central object.

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