团间介质对电离的重要性：Zeta Pup风中O VI的形成
On the Importance of the Interclump Medium for Superionization: O VI Formation in the Wind of Zeta Pup
摘要：
我们已经研究了超电离和X射线线形成的Zeta Pup光谱使用我们的新的恒星大气代码（XCMFGEN），可用于同时分析光学，紫外和X射线观测。在这里，我们提出的O VI 1111032，1038双重形成的结果。我们的模拟，支持简单的理论计算，表明，丛生风模型，假设无效的interclump空间不能重现所观察到的O VI配置文件。然而，如果空隙由低密度气体填充，则可以产生足够的OVI。O VI的重组在致密材料中是非常有效的，但在稀薄的块间区域中可以保持可观察到的O VI量。我们还发现，不同的紫外线共振线是敏感的不同的密度制度在Zeta Pup：C IV几乎完全形成的densitives区域内，而大部分的O VI之间的团块。NV是一个中间的情况下，从稀薄气体和团块的贡献。
英文摘要：
We have studied superionization and X-ray line formation in the spectra of Zeta Pup using our new stellar atmosphere code (XCMFGEN) that can be used to simultaneously analyze optical, UV, and X-ray observations. Here, we present results on the formation of the O VI ll1032, 1038 doublet. Our simulations, supported by simple theoretical calculations, show that clumped wind models that assume void in the interclump space cannot reproduce the observed O VI profiles. However, enough O VI can be produced if the voids are filled by a low density gas. The recombination of O VI is very efficient in the dense material but in the tenuous interclump region an observable amount of O VI can be maintained. We also find that different UV resonance lines are sensitive to different density regimes in Zeta Pup : C IV is almost exclusively formed within the densest regions, while the majority of O VI resides between clumps. N V is an intermediate case, with contributions from both the tenuous gas and clumps.
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