X射线辐照和盘状耀斑对年轻恒星[ NeII ] 12.8微米辐射的影响
Effects of X-ray irradiation and disk flaring on the [NeII] 12.8 micron emission from young stellar objects
摘要：
在几个年轻恒星天体（YSO）的光谱中，观测到了12.8 μ m的[Ne II]精细结构发射线。这条线被认为是由温暖的原行星盘大气的X射线辐射产生的，然而[Ne II]光度和测量的X射线光度之间的观测相关性显示出很大的散射。这样的传播限制了这条线作为盘的气相探针的实用性，因为几位作者已经建议流出物的污染作为观察到的散射的可能原因。在这项工作中，我们探讨的可能性，而不是由不同的星盘参数所造成的观测到的[Ne II]光度的大变化。特别是，我们研究的照射源的硬度和结构（耀斑）的磁盘上的[Ne II] 12.8微米线的光度和光谱轮廓的影响。我们发现，改变这些参数确实可以导致高达一个数量级的变化，在发射光度，这可能会解释观察到的散射，虽然我们的模型预测有点小的光度比最近报道的其他作者谁观察到的线与斯皮策太空望远镜。我们的模型还表明，光谱的硬度只有一个有限的（不可检测的）线轮廓上的影响，而在耀斑的磁盘功率的变化显着影响的[Ne II]发射区域的大小，因此，它的线轮廓。特别是，我们认为，广泛的线配置文件为中心的恒星径向速度可能是指示扁平的磁盘看到在大倾角。
英文摘要：
The [Ne II] fine-structure emission line at 12.8 micron has been detected in several young stellar objects (YSO) spectra. This line is thought to be produced by X-ray irradiation of the warm protoplanetary disk atmospheres, however the observational correlation between [Ne II] luminosities and measured X-ray luminosities shows a large scatter. Such spread limits the utility of this line as a probe of the gaseous phase of disks, as several authors have suggested pollution by outflows as a probable cause of the observed scatter. In this work we explore the possibility that the large variations in the observed [Ne II] luminosity may be caused instead by different star-disk parameters. In particular we study the effects that the hardness of the irradiating source and the structure (flaring) of the disk have on the luminosity and spectral profile of the [Ne II] 12.8 micron line. We find that varying these parameter can indeed cause up to an order of magnitude variation in the emission luminosities which may explain the scatter observed, although our models predict somewhat smaller luminosities than those recently reported by other authors who observed the line with the Spitzer Space Telescope. Our models also show that the hardness of the spectrum has only a limited (undetectable) effect on the line profiles, while changes in the flaring power of the disk significantly affect the size of the [Ne II] emission region and, as a consequence, its line profile. In particular we suggest that broad line profiles centred on the stellar radial velocity may be indicative of flat disks seen at large inclination angles.
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