Hard X-ray emission from a flare-related jet
Hard X-ray emission from a flare-related jet
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DOI：
10.1051/0004-6361/200911876
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发表时间：
2008-09
影响因子：
6.5
通讯作者：
H. Bain;L. Fletcher
中科院分区：
文献类型：
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作者：
H. Bain;L. Fletcher
目标。我们的目标是了解发生在2002年8月22日的喷流事件的物理条件，特别注意喷流材料中的非热电子的证据。方法.我们调查的耀斑脉冲阶段使用多波长观测过渡区和日冕探测器（TRACE）和Ramaty高能量光谱成像仪（RHESSI）卫星任务，和地面的Nobeyama射电日像仪（NoRH）和射电偏振仪（NoRP）。结果我们报告我们认为是第一次观察到硬X射线发射形成的日冕喷流。我们目前的无线电观测证实了非热电子在这个时候存在的射流。事件的演变是最好的磁重联喷流模型相比，新兴的磁场与预先存在的日冕场相互作用。我们计算出的表观射流速度约为500 km s-1，这与模型预测的由$\vec{J}\times\vec{B}$力加速的射流材料一致，导致阿尔芬速度（约100-1000 km s-1）的射流速度。
Aims. We aim to understand the physical conditions in a jet event which occurred on the 22nd of August 2002, paying particular attention to evidence for non-thermal electrons in the jet material. Methods. We investigate the flare impulsive phase using multiwavelength observations from the Transition Region and Coronal Explorer (TRACE) and the Reuven Ramaty High Energy Spectroscopic Imager (RHESSI) satellite missions, and the ground-based Nobeyama Radioheliograph (NoRH) and Radio Polarimeters (NoRP). Results. We report what we believe to be the first observation of hard X-ray emission formed in a coronal jet. We present radio observations which confirm the presence of non-thermal electrons present in the jet at this time. The evolution of the event is best compared with the magnetic reconnection jet model in which emerging magnetic field interacts with the pre-existing coronal field. We calculate an apparent jet velocity of ~500 km s -1 which is consistent with model predictions for jet material accelerated by the $\vec{J}\times\vec{B}$ force resulting in a jet velocity of the order of the Alfven speed (~100–1000 km s -1 ).