Star Formation and Dissipation in Galactic Discs
Disc galaxy evolution models may be classified according to the relative importance of star formation and dissipation in the disc gas. We discuss how the observed distribution of stars and of metals in galactic discs may be used to assess the degree of dissipation in the gas. We show that in order for viscously induced radial flows to have been important in the evolution of disc galaxies the timescale for the gas to dissipate its energy associated with local random motions must be ~ 107 years. Possible sources of dissipation in the disc gas are briefly discussed.
KeywordsAngular Momentum Star Formation Radial Flow Galactic Disc Disc Galaxy
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