ANALYSIS AND MODELING OF TWO FLARE LOOPS OBSERVED BY AIA AND EIS
ANALYSIS AND MODELING OF TWO FLARE LOOPS OBSERVED BY AIA AND EIS
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DOI：
10.1088/0004-637x/758/1/52
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发表时间：
2012-05
期刊：
影响因子：
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通讯作者：
Y. Li;J. Qiu;M. Ding
中科院分区：
文献类型：
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作者：
Y. Li;J. Qiu;M. Ding
我们分析和模拟了SDO/AIA和Hinode/EIS观测到的一个M1.0耀斑，以研究耀斑环如何被加热和随后的演化。耀斑是由两个独特的环系统在极紫外（EUV）图像观察。在这些环脚的UV 1600 μ m发射呈现出快速上升，随后由大气成像组件（AIA）和EUV成像光谱仪（EIS）观察到的不同EUV通道中的增强发射。这种行为表明脉冲能量存款和随后的反应，在覆盖日冕循环演变通过不同的温度。利用我们最近发展的方法，分别从两个环系统的紫外光变曲线的快速上升推导出经验加热函数，将它们看作两个截面积为5″ × 5″的大环，并利用EBTEL模型计算了环中等离子体的演化。我们计算的合成EUV光曲线，其中，与模型的限制，合理地同意在多个AIA通道和EIS线获得的观察到的光曲线：它们显示出相同的演变趋势和它们的幅度是可比的两个因素。此外，我们还比较了计算的平均焓流速度与多普勒频移测量EIS在两个循环的衰减阶段。我们的研究结果表明，这两个不同的循环具有不同的加热功能，从他们的足迹紫外线发射推断，结合他们的不同长度测量成像观测，引起不同的日冕等离子体演化模式捕获的模型和观测。
We analyze and model an M1.0 flare observed by SDO/AIA and Hinode/EIS to investigate how flare loops are heated and evolve subsequently. The flare is composed of two distinctive loop systems observed in extreme ultraviolet (EUV) images. The UV 1600 Å emission at the feet of these loops exhibits a rapid rise, followed by enhanced emission in different EUV channels observed by the Atmospheric Imaging Assembly (AIA) and the EUV Imaging Spectrometer (EIS). Such behavior is indicative of impulsive energy deposit and the subsequent response in overlying coronal loops that evolve through different temperatures. Using the method we recently developed, we infer empirical heating functions from the rapid rise of the UV light curves for the two loop systems, respectively, treating them as two big loops with cross-sectional area of 5″ by 5″, and compute the plasma evolution in the loops using the EBTEL model. We compute the synthetic EUV light curves, which, with the limitation of the model, reasonably agree with observed light curves obtained in multiple AIA channels and EIS lines: they show the same evolution trend and their magnitudes are comparable by within a factor of two. Furthermore, we also compare the computed mean enthalpy flow velocity with the Doppler shift measurements by EIS during the decay phase of the two loops. Our results suggest that the two different loops with different heating functions as inferred from their footpoint UV emission, combined with their different lengths as measured from imaging observations, give rise to different coronal plasma evolution patterns captured both in the model and in observations.