Book contents
- Frontmatter
- Contents
- List of contributors
- Preface
- Part I Abundances in the Galaxy: field stars
- Part II Abundances in the Galaxy: Galactic stars in clusters, bulges and the centre
- Part III Observations – abundances in extragalactic contexts
- Part IV Stellar populations and mass functions
- Part V Physical processes at high metallicity
- Part VI Formation and evolution of metal-rich stars and stellar yields
- Part VII Chemical and photometric evolution beyond Solar metallicity
- 43 Models of the Solar vicinity: the metal-rich stage
- 44 Chemical-evolution models of ellipticals and bulges
- 45 Chemical evolution of the Galactic bulge
- 46 How do galaxies become metal-rich? An examination of the yield problem
- 47 Abundance patterns: thick and thin disks
- 48 Formation and evolution of the Galactic bulge: constraints from stellar abundances
47 - Abundance patterns: thick and thin disks
Published online by Cambridge University Press: 02 December 2009
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Book contents
- Frontmatter
- Contents
- List of contributors
- Preface
- Part I Abundances in the Galaxy: field stars
- Part II Abundances in the Galaxy: Galactic stars in clusters, bulges and the centre
- Part III Observations – abundances in extragalactic contexts
- Part IV Stellar populations and mass functions
- Part V Physical processes at high metallicity
- Part VI Formation and evolution of metal-rich stars and stellar yields
- Part VII Chemical and photometric evolution beyond Solar metallicity
- 43 Models of the Solar vicinity: the metal-rich stage
- 44 Chemical-evolution models of ellipticals and bulges
- 45 Chemical evolution of the Galactic bulge
- 46 How do galaxies become metal-rich? An examination of the yield problem
- 47 Abundance patterns: thick and thin disks
- 48 Formation and evolution of the Galactic bulge: constraints from stellar abundances
Summary
We study the effect of assuming different formation timescales for the thick and thin disks on the variation of the abundance ratios of several elements with metallicity. We show that, if the thin disk was formed on a onger timescale (≃7 Gyr) than the thick disk (≃0.8 Gyr), the abundance ratio shifts between the thick and thin disk, as a function of the metallicity, can be well explained. Moreover, these observations offer a powerful constraint on stellar yields in general (massive stars, low- and intermediate-mass stars, and SN Ia) and their dependence on metallicity.
- Type
- Chapter
- Information
- The Metal-Rich Universe , pp. 454 - 459Publisher: Cambridge University PressPrint publication year: 2008