A Model of Double Coronal Hard X-Ray Sources in Solar Flares
A Model of Double Coronal Hard X-Ray Sources in Solar Flares
复制标题
太阳耀斑中双日冕硬X射线源模型
DOI：
10.3847/1538-4357/ac731b
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发表时间：
2022-01
期刊：
影响因子：
--
通讯作者：
Joe Giacalone
中科院分区：
文献类型：
--
作者：
Xiangliang Kong;Jing Ye;Bin Chen;Fan Guo;Chengcai Shen;Xiaocan Li;Sijie Yu;Yao Chen;Joe Giacalone
在太阳耀斑期间，RHESSI观测到了一些双日冕X射线源，其中两个源位于推断的重联位置的不同侧。然而，这些发射X射线的电子是在何处以及如何被加速的仍然不清楚。
A number of double coronal X-ray sources have been observed during solar flares by RHESSI, where the two sources reside at different sides of the inferred reconnection site. However, where and how these X-ray-emitting electrons are accelerated remains unclear. Here we present the first model of the double coronal hard X-ray (HXR) sources, where electrons are accelerated by a pair of termination shocks driven by bidirectional fast reconnection outflows. We model the acceleration and transport of electrons in the flare region by numerically solving the Parker transport equation using velocity and magnetic fields from the macroscopic magnetohydrodynamic simulation of a flux rope eruption. We show that electrons can be efficiently accelerated by the termination shocks and high-energy electrons mainly concentrate around the two shocks. The synthetic HXR emission images display two distinct sources extending to >100 keV below and above the reconnection region, with the upper source much fainter than the lower one. The HXR energy spectra of the two coronal sources show similar spectral slopes, consistent with the observations. Our simulation results suggest that the flare termination shock can be a promising particle acceleration mechanism in explaining the double-source nonthermal emissions in solar flares.
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