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| Paper: |
The Chemical Evolution of our Galaxy |
| Volume: |
317, Milky Way Surveys: The Structure and Evolution of Our Galaxy |
| Page: |
337 |
| Authors: |
Matteucci, F. |
| Abstract: |
I first review the basic ingredients necessary to build chemical evolution models for the Milky Way galaxy. Then I discuss how to infer important constraints on the mechanisms of formation and evolution of our Galaxy by comparison between model results and observations. In particular, I focus on the stellar abundances which recently have reached an high level of accuracy. Both common and specific conclusions from the different chemical evolution models existing in the literature are presented. Common conclusions suggest that the Milky Way thin disk formed inside-out and on much longer timescales than the halo, the bulge and the thin disk. This implies that the gas forming the thin disk must have been accreted from the intergalactic medium. Some specific models predict a gap in the star formation rate just before the formation of the thin disk, as it seems to be indicated by a gap in some observed abundance ratios. |
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