The chemical evolution of disk galaxies

Details The chemical evolution of disk galaxies The chemical evolution of disk galaxies

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993azh....70..277s&link_type=abstract

Astronomicheskij Zhurnal (ISSN 0004-6299), vol. 70, no. 2, p. 277-291.

Astronomy and Astrophysics

Astronomy

1

Brightness Distribution, Chemical Evolution, Disk Galaxies, Galactic Evolution, Gas Dynamics, Angular Momentum, Radial Flow, Star Formation

Scientific paper

The chemical evolution of the gaseous subsystem of galactic disks is considered within the framework of the model of Lin and Pringle (1987). It is assumed that in addition to the star formation process in a disk, there exists a radial flow of gas in its plane. The radial fluxes are caused by a large-scale gravitational instability which gives rise to a complicated picture of interacting density waves. Typical time scales of star formation and gas redistribution are argued to be comparable. Specific galaxies (M31, the Milky Way, M33, and M81) are used to illustrate the good correlation between theory and observations, given a reasonable choice of parameters.

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