Chemical self-enrichment of HII regions by the Wolf-Rayet phase of an 85 M star

Danica Kröger, Gerhard Hensler, Tim Freyer

Veröffentlichungen: Beitrag in FachzeitschriftArtikelPeer Reviewed

Abstract

It is clear from stellar evolution and from observations of WR stars that massive stars are releasing metal-enriched gas through their stellar winds in the Wolf-Rayet phase. Although HII region spectra serve as diagnostics to determine the present-day chemical composition of the interstellar medium, it is far from being understood to what extent the HII gas is already contaminated by chemically processed stellar wind. Therefore, we analyzed our models of radiative and wind bubbles of an isolated 85 Mž star with solar metallicity (Krošger et al. 2006, A&A, in preparation) with respect to the chemical enrichment of the circumstellar HII region. Plausibly, the hot stellar wind bubble (SWB) is enriched with 14N during the WN phase and even much higher with 12C and 16O during the WC phase of the star. During the short period that the 85 Mž star spends in the WC stage enriched SWB material mixes with warm HII gas of solar abundances and thus enhances the metallicity in the HII region. However, 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. Important issues from the presented study comprise a steeper radial gradient of C than O and a decreasing effect of self-enrichment for metal-poor galaxies. Œ ESO 2006.
OriginalspracheEnglisch
Seiten (von - bis)5-8
Seitenumfang4
FachzeitschriftAstronomy & Astrophysics
Jahrgang450
Ausgabenummer1
DOIs
PublikationsstatusVeröffentlicht - 2006

ÖFOS 2012

  • 103003 Astronomie

Fingerprint

Untersuchen Sie die Forschungsthemen von „Chemical self-enrichment of HII regions by the Wolf-Rayet phase of an 85 M star“. Zusammen bilden sie einen einzigartigen Fingerprint.

Zitationsweisen