Evidence for and Analysis of Multiple Hidden Coronal Strands in Cross-sectional Emission Profiles: Further Results from NASA’s High-resolution Solar Coronal Imager
Evidence for and Analysis of Multiple Hidden Coronal Strands in Cross-sectional Emission Profiles: Further Results from NASA’s High-resolution Solar Coronal Imager
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横截面发射剖面中多个隐藏日冕链的证据和分析：美国宇航局高分辨率太阳日冕成像仪的进一步结果
DOI：
10.3847/1538-4357/abb60a
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发表时间：
2020
期刊：
影响因子：
--
通讯作者：
A. Winebarger
中科院分区：
文献类型：
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作者：
T. Williams;R. Walsh;H. Peter;A. Winebarger
先前利用NASA高分辨率日冕成像仪（Hi-C 2.1） 172 Å观测结果的工作表明，即使在数据集中可用的空间尺度增加的情况下，可能仍有证据表明日冕结构尚未完全解决。在这项后续研究中，冠状链的横截面切片在hi - c2.1视场中被拍摄。根据先前的环宽研究，本底发射被移除以隔离日冕束。由此产生的强度变化是通过使用非线性最小二乘曲线拟合方法同时拟合多个高斯曲线来再现的。总共检查了183个高斯分布，以寻找数据中暗示的可能结构。对每个高斯分布确定半最大值时的全宽度，然后对其进行整理和分析。最常见的结构宽度约为450-575公里，其中47%的链宽度低于美国宇航局太阳动力学天文台大气成像组件（AIA）的分辨率（600-1000公里）。只有17%位于AIA像素宽度（435公里）以下，只有6%位于Hi-C 2.1分辨率尺度（≈220-340公里）。这些结果表明，Hi-C 2.1观测到的非高斯形状的截面发射曲线是沿集成瞄准线上可以被分解的多条线的结果，而不是更精细的亚分辨率元素的结果。
Previous work utilizing NASA’s High-resolution Coronal Imager (Hi-C 2.1) 172 Å observations revealed that, even at the increased spatial scales available in the dataset, there may be evidence for coronal structures that are still not fully resolved. In this follow-up study, cross-section slices of coronal strands are taken across the Hi-C 2.1 field of view. Following previous loop-width studies, the background emission is removed to isolate the coronal strands. The resulting intensity variations are reproduced by simultaneously fitting multiple Gaussian profiles using a nonlinear least-squares curve-fitting method. In total, 183 Gaussian profiles are examined for possible structures that are hinted at in the data. The full width at half maximum is determined for each Gaussian, which are then collated and analyzed. The most frequent structural widths are ≈450–575 km with 47% of the strand widths beneath NASA’s Solar Dynamics Observatory Atmospheric Imaging Assembly (AIA) resolving scale (600–1000 km). Only 17% reside beneath an AIA pixel width (435 km) with just 6% of the strands at the Hi-C 2.1 resolving scale (≈220–340 km). These results suggest that non-Gaussian shaped cross-sectional emission profiles observed by Hi-C 2.1 are the result of multiple strands along the integrated line of sight that can be resolved, rather than being the result of even finer sub-resolution elements.
DOI：
10.3847/1538-4357/aa5ff9
发表时间：
2017-03
期刊：
The Astrophysical Journal
影响因子：
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作者：
D. Pontin;M. Janvier;S. K. Tiwari;K. Galsgaard;A. Winebarger;J. Cirtain
通讯作者：
D. Pontin;M. Janvier;S. K. Tiwari;K. Galsgaard;A. Winebarger;J. Cirtain