Very massive binaries in R 136
Very massive binaries in R 136
复制标题
R 136 中非常庞大的二进制文件
DOI：
10.1017/s174392131101115x
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发表时间：
2010
期刊：
影响因子：
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通讯作者：
A. Moffat
中科院分区：
文献类型：
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作者：
A. Chené;O. Schnurr;P. Crowther;E. Lajus;A. Moffat
摘要 正如最近的观测表明，发光、富氢的 WN5-7h 星（以及它们的不太极端的近亲 O3f/WN6 星）是已知质量最大的主序星。然而，还没有足够多的大质量恒星被可靠地称重以产生上部初始质量函数（IMF）的清晰图像。因此，我们对 LMC 中 R136 中的四个新的 O3f/WN6 和 WN5-7h 双星在双子座南区的 GMOS 中进行了重复的高质量光谱分析，分别推导出这两个组分的开普勒轨道，从而直接确定它们的质量。我们还监测了双星候选者和其他以前未测量过的恒星，以增加可以直接称重的超大质量恒星的数量。
Abstract As recent observations have shown, luminous, hydrogen-rich WN5-7h stars (and their somewhat less extreme cousins, O3f/WN6 stars) are the most massive main-sequence stars known. However, not nearly enough very massive stars have been reliably weighed to yield a clear picture of the upper initial-mass function (IMF). We therefore have carried out repeated high-quality spectroscopy of four new O3f/WN6 and WN5-7h binaries in R136 in the LMC with GMOS at Gemini-South, to derive Keplerian orbits for both components, respectively, and thus to directly determine their masses. We also monitored binary candidates and other, previously unsurveyed stars, to increase the number of very massive stars that can be directly weighed.