PROPERTIES OF MASSIVE STARS IN VVV CLUSTERS

被引：0

作者：

Herve, A. ^{[1
]}

Martins, F. ^{[2
]}

Chene, A. -N. ^{[3
]}

Bouret, J. -C. ^{[4
]}

Borrissova, J. ^{[5
]}

机构：

[1] Astron Inst ASCR, Friova 298, Ondejov 25165, Czech Republic

[2] Univ Montpellier, LUPM, CNRS, F-34095 Montpellier, France

[3] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA

[4] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France

[5] Univ Valparaiso, Inst Fis & Astron, Playa Ancha, Chile

来源：

PHYSICS OF EVOLVED STARS: A CONFERENCE DEDICATED TO THE MEMORY OF OLIVIER CHESNEAU | 2015年 / 71-72卷

关键词：

D O I：

10.1051/eas/1571079

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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. 2011). 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.

引用

页码：337 / 338

页数：2

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