Properties of massive stars in four clusters of the VVV survey

被引：5
|
作者：
Herve, A. [1 ,2 ]
Martins, F. [2 ]
Chene, A. -N. [3 ]
Bouret, J. -C. [4 ]
Borissova, J. [5 ,6 ,7 ]
机构：
[1] Astron Inst ASCR, Fricova 298, Ondrejov 25165, Czech Republic
[2] Univ Montpellier, CNRS, LUPM, Pl Eugene Bataillon, F-34095 Montpellier, France
[3] Gemini Observ, Northern Operat Ctr, 670 N Aohoku Pl, Hilo, HI 96720 USA
[4] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France
[5] Univ Valparaiso, Inst Fis & Astron, Av Gran Bretana 1111a,Casilla 5030, Playa Ancha, Chile
[6] Milky Way Millennium Nucleus, Av Vicuna Mackenna 4860, Santiago 7820436, Chile
[7] Millenium Inst Astrophys, MAS, Av Gran Bretana 1111,Casilla 5030, Valparaiso, Chile
来源：
NEW ASTRONOMY | 2016年 / 45卷
关键词：
Galaxy: open clusters and associations; Stars: massive; Stars: Wolf-Rayet; SPECTRAL ATLAS; STELLAR; WIND; CANDIDATES; SUPERGIANT; EVOLUTION; CLUMPS; HOT;
D O I：
10.1016/j.newast.2015.10.009
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. We present an analysis of massive stars in four of these new clusters. Our aim is to provide constraints on stellar evolution and to better understand the relation between different types of massive stars. We use the radiative transfer code CMFGEN to analyse K-band spectra of twelve stars with spectral types ranging from O and B to WN and WC. We derive the stellar parameters of all targets as well as surface abundances for a subset of them. In the Hertzsprung Russell diagram, the Wolf-Rayet stars are more luminous or hotter than the O stars. From the log(C/N) log(C/He) diagram, we show quantitatively that WN stars are more chemically evolved than O stars, WC stars being more evolved than WN stars. Mass loss rates among Wolf-Rayet stars are a factor of 10 larger than for O stars, in agreement with previous findings. (C) 2015 Elsevier B.V. All rights reserved.
引用
收藏
页码：84 / 91
页数：8
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