The chemical evolution of a spiral galaxy disks

Details The chemical evolution of a spiral galaxy disks The chemical evolution of a spiral galaxy disks

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992ap%26ss.190..243c&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 190, no. 2, April 1992, p. 243-256.

Astronomy and Astrophysics

Astrophysics

1

Chemical Evolution, Galactic Evolution, Galactic Structure, Spiral Galaxies, Astronomical Models, Dark Matter, Hubble Constant, Interstellar Matter

Scientific paper

The results of computing the evolution of a disk subsystem of a spiral galaxy taking into account radial gradients of chemical elements (D, He-4, C-12, C-13, N-14, O-16, Li-7, Fe) are presented. It is shown that the flow of intergalactic matter accreting on to the galaxy results in smoothing the radial gradients of gas and chemical elements, especially at the latest stage of the evolution. The final gradients depend weakly on the age of the galaxy and value of the Hubble constant h. The best agreement between calculated and observed abundance of He-4 is revealed if the primordial yield is Y(0) = 0.25. The small decrease of the primordial deuterium abundance confirms the conclusion that the baryon density parameter is small: Omega(b) h super 250 not greater than 1. Therefore, the nature of dark matter should be nonbaryonic.

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