TRACING THE CHROMOSPHERIC AND CORONAL MAGNETIC FIELD WITH AIA, IRIS, IBIS, AND ROSA DATA
TRACING THE CHROMOSPHERIC AND CORONAL MAGNETIC FIELD WITH AIA, IRIS, IBIS, AND ROSA DATA
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DOI：
10.3847/0004-637x/826/1/61
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发表时间：
2016-02
期刊：
影响因子：
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通讯作者：
M. Aschwanden;K. Reardon;D. Jess
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文献类型：
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作者：
M. Aschwanden;K. Reardon;D. Jess
本研究的目的是探讨活动区的磁模拟的色球图像的适用性。我们使用高分辨率图像（），来自干涉二维光谱仪的Ca ii 8542线，太阳大气中的快速振荡仪器的Hα 6563线，界面区域成像光谱仪的2796线，与非-从这些色球图像中获得的潜在磁场模型与从日冕大气成像组件图像中获得的潜在磁场模型进行了比较，（171等）和色球层（304 nm）波长。曲线-线性结构自动跟踪在这些图像中的OCCITAL-2代码，我们向前拟合的磁场线计算的垂直电流近似非线性力自由场代码。我们发现色球图像：（1）显示出清晰的曲线-线性结构（2）这些曲线-线性结构通过-7°的中值未对准角与最佳拟合解场对准;（3）由日冕资料计算的自由能可能比色球资料计算的自由能低-4倍;（4）色球特征的高度范围仅限于km，而日冕特征在h = 35，000 km处被探测到;（5）等离子体-β参数适用于所有被追踪的特征。我们的结论是，色球图像揭示了重要的磁结构，是互补的日冕图像，需要包括在全面的磁场模型，这是目前没有容纳在标准NLFFF代码。
The aim of this study is to explore the suitability of chromospheric images for magnetic modeling of active regions. We use high-resolution images ( ), from the Interferometric Bidimensional Spectrometer in the Ca ii 8542 Å line, the Rapid Oscillations in the Solar Atmosphere instrument in the Hα 6563 Å line, the Interface Region Imaging Spectrograph in the 2796 Å line, and compare non-potential magnetic field models obtained from those chromospheric images with those obtained from images of the Atmospheric Imaging Assembly in coronal (171 Å, etc.) and in chromospheric (304 Å) wavelengths. Curvi-linear structures are automatically traced in those images with the OCCULT-2 code, to which we forward-fitted magnetic field lines computed with the Vertical-current Approximation Nonlinear Force Free Field code. We find that the chromospheric images: (1) reveal crisp curvi-linear structures (fibrils, loop segments, spicules) that are extremely well-suited for constraining magnetic modeling; (2) that these curvi-linear structures are field-aligned with the best-fit solution by a median misalignment angle of –7°; (3) the free energy computed from coronal data may underestimate that obtained from cromospheric data by a factor of –4, (4) the height range of chromospheric features is confined to km, while coronal features are detected up to h = 35,000 km; and (5) the plasma-β parameter is for all traced features. We conclude that chromospheric images reveal important magnetic structures that are complementary to coronal images and need to be included in comprehensive magnetic field models, something that is currently not accomodated in standard NLFFF codes.