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
34 - The observable metal-enrichment of radiation-driven-plus-wind-blown H II regions in the Wolf–Rayet stage
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
From stellar-evolution models and from observations of Wolf–Rayet stars it is known that massive stars are releasing metal-enriched gas during their Wolf–Rayet phase by means of strong stellar winds. Although H ii-region spectra serve as diagnostics to determine the present-day chemical composition of the interstellar medium, it is not yet reliably known to what extent the diagnostic H ii gas is already contaminated by chemically processed stellar-wind matter. In a recent paper, we therefore analyzed our models of radiation-driven and wind-blown H ii bubbles around an isolated 85M⊙ star of originally Solar metallicity with respect to its chemical abundances. Although the hot stellar-wind bubble (SWB) is enriched with 14N during the WN phase and even more so with 12C and 16O during the WC phase of the star, we found that at the end of the stellar lifetime the mass ratios of the traced elements N and O in the warm ionized gas are insignificantly higher than Solar, whereas an enrichment of 22% above Solar is found for C. The transport of enriched elements from the hot SWB to the cool gas occurs mainly by means of mixing of hot gas with cooler at the back side of the SWB shell.
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- The Metal-Rich Universe , pp. 327 - 331Publisher: Cambridge University PressPrint publication year: 2008
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