On the Importance of the Interclump Medium for Superionization: O VI Formation in the Wind of ζ Puppis
On the Importance of the Interclump Medium for Superionization: O VI Formation in the Wind of ζ Puppis
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论簇间介质对超电离的重要性： ze 风中的 O VI 形成
DOI：
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发表时间：
2008
期刊：
影响因子：
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通讯作者：
David H. Cohen
中科院分区：
文献类型：
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作者：
J. Zsargó;D. Hillier;J. Bouret;Thierry Lanz;M. Leutenegger;David H. Cohen
我们用我们的新的恒星大气程序(XCMFGEN)研究了ζPUP光谱中的上位化和X射线谱线的形成，该程序可以同时分析光学、紫外和X射线观测。在这里，我们给出了关于OVIλλ1032,1038二重态形成的结果。我们的模拟得到了简单的理论计算的支持，表明假设星团间空间为空洞的团状风模型不能再现观测到的OVI廓线。然而，如果用低密度气体填充空隙，则可以产生足够的OVI。在致密的物质中，O-VI的复合是非常有效的，但在稀疏的团簇间区域，O-VI可以保持可观的量。我们还发现，在ζPUP中，不同的UV共振线对不同的密度区域是敏感的：C IV几乎完全形成在最密集的区域，而O VI主要存在于团簇之间。N-V是一种中间情况，既有稀薄气体的贡献，也有团块的贡献。
We have studied superionization and X-ray line formation in the spectra of ζ 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 λλ1032, 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 ζ 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.