Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993arep...37..144s&link_type=abstract
Astronomy Reports, Volume 37, Issue 2, March 1993, pp.144-151
Astronomy and Astrophysics
Astronomy
Scientific paper
We consider the chemical evolution of the gaseous component of a galactic disk using the model of Lin and Pringle (1987). We assume that in addition to star formation in the disk, radial gas flow occurs in its plane. The reason for the radial flows is large-scale gravitational instability, producing a complicated pattern of interacting density waves capable of transporting angular momentum. We also assume that the characteristic times of star formation and gas redistribution are comparable to each other. We find a self-similar solution for the problem. Using specific galaxies (M 31, M 33, M 81, and our Galaxy) as examples, we demonstrate good agreement between the predictions of the theory and observational data for a reasonable choice of the parameters. Agreement between theory and observations is reached under the condition that the gas has been preliminarily enriched to Z = 0.25Z_sun_ in the predisk stage.
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