论文标题
对大麦芽云中C II排放线星星的调查。 ii。最终结果和[WC]光谱中C II发射的起源
A Survey for C II Emission-Line Stars in the Large Magellanic Cloud. II. Final Results and the Origin of C II Emission in [WC] Spectra
论文作者
论文摘要
我们介绍了具有C II 7231，7236发射线的大麦芽云（LMC）中恒星的成像和光谱搜索的最终结果。目的是识别和研究[WC11]恒星，低质量狼射线序列中最酷的恒星以及行星星云的中央恒星的子集，其中C II线尤为突出。最近发现LMC [WC11]的偶然性发现增加了这些物体虽然难以识别，但实际上可能比以前认为的更为普遍。在这项调查中发现了这个罕见班级的几个新成员。但是，现在似乎很清楚，这些恒星中有大量恒星并未隐藏在一般的[WC]人群中。我们指出，在我们的光谱中观察到的C II双压力集强度比将物体整齐地分为两个不同的组，而C II发射可能源自恒星风或周围的星云。 C II排放机制的物理学正确解释了这种分叉。对于大多数对象，建议使用光谱子类型。现在可用于这些对象的众多光谱线索应促进未来的详细建模。
We present the final results of an imaging and spectroscopic search for stars in the Large Magellanic Cloud (LMC) with C II 7231, 7236 emission lines. The goal is to identify and study [WC11] stars, the coolest of the low-mass Wolf-Rayet sequence, and a subset of central stars of planetary nebulae where the C II lines are known to be especially prominent. A recent serendipitous discovery of an LMC [WC11] raised the possibility that these objects, although difficult to identify, might in fact be more common than previously believed. Several new members of this rare class have been found in this survey. It now seems clear, however, that a significant number of these stars are not hiding amongst the general [WC] population. We point out that the C II doublet intensity ratio observed in our spectra proves to neatly divide the objects into two distinct groups, with the C II emission likely originating from either the stellar wind or a surrounding nebula. The physics of the C II emission mechanism correctly explains this bifurcation. Spectral subtypes are suggested for most of the objects. The numerous spectroscopic clues now available for these objects should facilitate future detailed modeling.
