| Issue |
EAS Publications Series
Volume 71-72, 2015
The Physics of Evolved Stars: A Conference Dedicated to the Memory of Olivier Chesneau
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|---|---|---|
| Page(s) | 337 - 338 | |
| Section | Modeling, Evolution | |
| DOI | https://doi.org/10.1051/eas/1571079 | |
| Published online | 01 December 2015 | |
E. Lagadec, F. Millour and T. Lanz (eds)
EAS Publications Series, 71–72 (2015) 337-338
Properties of Massive Stars in VVV Clusters
1 Astronomical Institue of the ASCR, Friova 298, 251 65 Ondejov, Czech Republic
2 LUPM, Université de Montpellier, CNRS, Place Eugène Bataillon, 34095 Montpellier, France
3 Gemini Observatory, Northern Operations Center, 670 North Aohoku Place, Hilo, HI 96720, USA
4 Aix Marseille Université, CNRS, LAM, UMR 7326, 13388 Marseille, France
5 Instituto de Física y Astronomía, U. de Valparaíso, Av. Gran Bretana 1111, Playa Ancha, 5030 Casilla, Chile
The evolution of massive stars is only partly understood. Observational constraints can be obtained from the study of massive stars located in young massive clusters. The ESO Public Survey VISTA Variables in the Via Lactea (VVV) discovered several new clusters hosting massive stars (Borrissova et al. [1]). We derive the stellar parameters of all targets as well as surface abundances for a subset of them. For the cluster with the largest number of objects, we establish firmly that the WN and WC stars were initially more massive than the O stars still present in the cluster.
© EAS, EDP Sciences, 2015