Flare-related Recurring Active Region Jets: Evidence for Very Hot Plasma
Flare-related Recurring Active Region Jets: Evidence for Very Hot Plasma
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DOI：
10.1007/s11207-018-1376-4
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发表时间：
2018-12
期刊：
影响因子：
2.8
通讯作者：
Sargam M. Mulay;S. Matthews;T. Hasegawa;G. del Zanna;H. Mason;T. Shimizu
中科院分区：
文献类型：
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作者：
Sargam M. Mulay;S. Matthews;T. Hasegawa;G. del Zanna;H. Mason;T. Shimizu
我们提出了一个与两个C级X射线耀斑相关的两个活动区喷流（AR喷流）的研究。周期性的同源喷流来自太阳黑子的北方边缘。我们使用Fexxiii（263.76）和Fexxiv（255.11）发射线的光谱观测，证实了这些喷流足点处的耀斑样温度。用发射测量轨迹方法得到了一个等温温度，结果表明在C3.0耀斑的衰变阶段温度降低（17.7 ~ 13.6 MK）。发现足点的电子数密度范围从使用Fexivline对比率。Fexxiv的非热速度范围为34 - 100 km/s，Fexxiii为51 - 89 km/s。利用大气成像组件（AIA）171毫米波通道计算了两股喷流的天平面速度。喷流足迹区的AIA光变曲线证实了两次X射线耀斑与喷流足迹发射之间的时空相关性。伽玛射线暴监测器（GBM）也证实了在其中一个耀斑的上升（峰值）阶段，在喷流足点区域有27（25）MK的超热等离子体，非热能为（）。从EIS得到的喷流足点区域的温度与从地球同步环境业务卫星（GOES）通量比得到的温度非常一致（在20%的不确定度内）。这些结果为耀斑相关喷流的足点处非常热的等离子体（）提供了明确的证据，并且它们证实了耀斑期间等离子体的加热和冷却。
We present a study of two active region jets (AR jets) that are associated with two C-class X-ray flares. The recurrent, homologous jets originated from the northern periphery of a sunspot. We confirm flare-like temperatures at the footpoints of these jets using spectroscopic observations of Fexxiii(263.76 Å) and Fexxiv(255.11 Å) emission lines. The emission measure loci method was used to obtain an isothermal temperature, and the results show a decrease (17.7 to 13.6 MK) in the temperature during the decay phase of the C 3.0 flare. The electron number densities at the footpoints were found to range fromtousing the Fexivline pair ratio. Nonthermal velocities were found to range from 34 – 100 km/s for Fexxivand 51 – 89 km/s for Fexxiii. The plane-of-sky velocities were calculated to beandfor the two jets using theAtmospheric Imaging Assembly(AIA) 171 Å channel. The AIA light curves of the jet footpoint regions confirmed the temporal and spatial correlation between the two X-ray flares and the jet footpoint emission. TheGamma-ray Burst Monitor(GBM) also confirmed superhot plasma of 27 (25) MK with a nonthermal energy of()in the jet footpoint region during the rise (peak) phase of one of the flares. The temperatures of the jet footpoint regions obtained from EIS agree very well (within an uncertainty of 20%) with temperatures obtained from theGeostationary Environmental Operational Satellite(GOES) flux ratios. These results provide clear evidence for very hot plasma () at the footpoints of the flare-related jets, and they confirm the heating and cooling of the plasma during the flares.