Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980mnras.191..195b&link_type=abstract
Monthly Notices of the Royal Astronomical Society, vol. 191, Apr. 1980, p. 195-206.
Astronomy and Astrophysics
Astronomy
32
Galactic Nuclei, Stellar Evolution, Stellar Mass Ejection, Astronomical Models, Elliptical Galaxies, Interstellar Matter, Numerical Integration, Spiral Galaxies, Supernovae
Scientific paper
The evolution of stellar mass loss in the central regions of ordinary galactic nuclei, both spiral and elliptical, is investigated to determine conditions under which stellar mass loss flows inwards rather than outwards as a supernova-driven galactic wind. It is shown that the presence of even a small quantity of gas in the nuclear region is sufficient to cause cooling and to allow the existence of a substantial region of inflow within the Galactic Center. The inflowing gas is assumed to conserve its angular momentum, and to lead to the formation of a dense, cold nuclear disk. The observed qualitative difference between nuclear activity in spiral and elliptical galaxies is attributed to the differences in the structure and evolution of nuclear disks formed by essentially the same process: inflowing stellar mass loss.
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