用IBIS：III高分辨率观测太阳色球层。Ca II K和Ca II 854.2 nm成像的比较
The solar chromosphere at high resolution with IBIS: III. Comparison of Ca II K and Ca II 854.2 nm imaging
摘要：
在Ca II H、Ca II K和H-α中获得的滤波图经常被用作太阳色球层的诊断。然而，这些不同线路中的典型滤波图之间的巨大差异的外观引起了人们对实际观察到的性质的质疑。我们调查缺乏明显的结构的磁起源，如纤维和斑点在磁盘上的钙II H和K的图像通过直接比较经典的钙II K滤波图的时间序列的光谱分辨钙II 854.2图像的空间和时间序列的干涉二维光谱仪（IBIS），考虑到光谱和空间拖尾的影响。我们发现，缺乏精细的磁性结构的钙II K过滤图，即使与最先进的过滤器，是由于观测效果。然而，在滤波图的时间演化中，纤维的签名仍然存在，特别是在网络元素周围的磁阴影的证据下。然而，钙II K滤波图并不能正确地反映色球层的高频行为。使用相同的分析，我们没有发现显着的色球签名在日出/SOT钙II H安静的太阳过滤图。由H-α和Ca II 854.2提供的图片显示了色球层的重要部分由磁性结构主导，似乎反映了太阳色球层的真实和本质性质。不能在空间或光谱上分辨的数据可能会歪曲色球层的行为.
英文摘要：
Filtergrams obtained in Ca II H, Ca II K and H-alpha are often employed as diagnostics of the solar chromosphere. However, the vastly disparate appearance between the typical filtergrams in these different lines calls into question the nature of what is actually being observed. We investigate the lack of obvious structures of magnetic origin such as fibrils and mottles in on-disk Ca II H and K images by directly comparing a temporal sequence of classical Ca II K filtergrams with a co-spatial and co-temporal sequence of spectrally resolved Ca II 854.2 images obtained with the Interferometric Bidimensional Spectrometer (IBIS), considering the effect of both the spectral and spatial smearing. We find that the lack of fine magnetic structuring in Ca II K filtergrams, even with the narrowest available filters, is due to observational effects. Signatures of fibrils remain however in the temporal evolution of the filtergrams, in particular with the evidence of magnetic shadows around the network elements. The Ca II K filtergrams do not appear, however, to properly reflect the high-frequency behavior of the chromosphere. Using the same analysis, we find no significant chromospheric signature in the Hinode/SOT Ca II H quiet-Sun filtergrams. The picture provided by H-alpha and Ca II 854.2, which show significant portions of the chromosphere dominated by magnetic structuring, appears to reflect the true and essential nature of the solar chromosphere. Data which do not resolve, spatially or spectrally, this aspect may misrepresent the behavior the chromosphere.
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