Other
Scientific paper
Apr 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...221..554t&link_type=abstract
Astrophysical Journal, Part 1, vol. 221, Apr. 15, 1978, p. 554-561. Research supported by the Alfred P. Sloan Foundation
Other
134
Abundance, Astronomical Models, Chemical Evolution, Galactic Evolution, Galactic Structure, Gravitational Collapse, Interstellar Gas, Kinematics, Metals, Spiral Galaxies, Stellar Evolution, Velocity Distribution
Scientific paper
The chemical evolution of two collapse models for the formation of disk galaxies is calculated in detail, and the results are compared with properties of our own and other spiral galaxies. The models show at least qualitative agreement with empirical stellar and interstellar abundance gradients and with color gradients in spiral galaxies. The outer parts of the model disks are also in general agreement with the metallicity and age distributions of stars in the solar neighborhood, and with correlations between metallicity and kinematics for nearby stars. It is concluded that the process of disk formation by gradual accumulation of gas into a plane may account in a natural way for many properties of disk galaxies. In general, gas flows within or from outside galaxies are expected to have very important effects on chemical evolution.
Larson Richard B.
Tinsley Beatrice M.
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