Models for WR and O Star Populations in Starbursts: New Developments and Applications to Large Samples of WR Galaxies

Details Models for WR and O Star Populations in Starbursts: New Developments and Applications to Large Samples of WR Galaxies Models for WR and O Star Populations in Starbursts: New Developments and Applications to Large Samples of WR Galaxies

1998-12-18

arxiv.org/abs/astro-ph/9812357v2

Astronomy and Astrophysics

Astrophysics

Invited talk, to appear in "Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies", Eds. K.A. van der Hucht, G. Koenigs

Scientific paper

We summarise recent developments on synthesis models for massive star populations with a particular emphasis on Wolf-Rayet (WR) stars. Quantitative analysis of the stellar content of WR galaxies are reviewed. Comparing observations of WR galaxies from various samples with synthesis models we derive constraints on their burst properties. The observations indicate very short burst periods and are generally compatible with a Salpeter IMF and a large upper mass cut-off. The use of the Hbeta equivalent width as an age indicator works well for WR galaxies. We briefly summarise comparisons of stellar populations in super star clusters which also provide useful contraints on evolutionary models for massive stars e.g. at very low metallicities inaccessible in the Local Group. In particular the observed WN and WC populations favour the high mass loss models of Meynet et al. (1994). Finally we review recent work on the origin of nebular HeII emission. From the new catalogue of WR galaxies and high excitation HII regions of Schaerer et al. (1998) we find a close relation between the presence of nebular HeII and WR stars. The analysis of individual WR galaxies including I Zw 18 supports the suggestion of Schaerer (1996) that hot WR stars are responsible for the hard ionizing flux.

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