Chemical Evolution of Galaxies and the Universe

Details Chemical Evolution of Galaxies and the Universe Chemical Evolution of Galaxies and the Universe

Apr 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aps..apr.h4004h&link_type=abstract

American Physical Society, April Meeting, April 28 - May 1, 2001 Washington, DC Bulletin of the American Physical Society, Vol.

Physics

Scientific paper

The chemical enrichment history of the Milky Way is determined by the yields of various sources of nucleosynthesis (AGB/WR stars, novae, supernovae, cosmic rays, etc) and the star formation rate (SFR), whose present-day value is of order a few solar masses per year. This SFR corresponds to a supernova rate of a few events per century. The SFR was significantly higher in the past, and the disk of the Milky Way began forming stars about 10 Gyrs ago. Well developed models of chemical evolution describe the increasing metal content of the interstellar medium and the evolving abundance pattern recorded in stars. But how does one apply the concepts of galactic chemical evolution to the universe as a whole, and what kind of observations should one use to constrain models of cosmic chemical evolution?

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