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
- 31 Stellar winds from Solar-metallicity and metal-rich massive stars
- 32 On the determination of stellar parameters and abundances of metal-rich stars
- 33 Are WNL stars tracers of high metallicity?
- 34 The observable metal-enrichment of radiation-driven-plus-wind-blown H II regions in the Wolf–Rayet stage
- 35 Metal-rich A-type supergiants in M31
- Part VI Formation and evolution of metal-rich stars and stellar yields
- Part VII Chemical and photometric evolution beyond Solar metallicity
31 - Stellar winds from Solar-metallicity and metal-rich massive stars
Published online by Cambridge University Press: 02 December 2009
- 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
- 31 Stellar winds from Solar-metallicity and metal-rich massive stars
- 32 On the determination of stellar parameters and abundances of metal-rich stars
- 33 Are WNL stars tracers of high metallicity?
- 34 The observable metal-enrichment of radiation-driven-plus-wind-blown H II regions in the Wolf–Rayet stage
- 35 Metal-rich A-type supergiants in M31
- Part VI Formation and evolution of metal-rich stars and stellar yields
- Part VII Chemical and photometric evolution beyond Solar metallicity
Summary
We discuss theoretical predictions and observational findings obtained for radiatively driven winds of massive stars, with emphasis on their dependence on metallicity. If these winds are not strongly clumped or the clumping properties are independent of metallicity z, theory and observations agree very well, and mass-loss rates and terminal velocities scale as Ṁ ∝ z0.62±015 and υ∞ ∝ z0.13, respectively. This dependence could be validated only for winds with Solar and subsolar abundances, due to the lack of supersolar-metallicity test cases. The actual values for the mass-loss rates are uncertain, due to unknown clumping properties of the wind, and currently accepted numbers might be overestimated by factors in between ∼2 and 10.
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- Chapter
- Information
- The Metal-Rich Universe , pp. 295 - 307Publisher: Cambridge University PressPrint publication year: 2008
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