Clear Evidence of Reconnection Inflow of a Solar Flare
Clear Evidence of Reconnection Inflow of a Solar Flare
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DOI：
10.1086/318053
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发表时间：
2001
期刊：
影响因子：
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通讯作者：
Takaaki Yokoyama;K. Akita;T. Morimoto;K. Inoue;Jeffrey Newmark
中科院分区：
文献类型：
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作者：
Takaaki Yokoyama;K. Akita;T. Morimoto;K. Inoue;Jeffrey Newmark
我们在1999年3月18日的一次耀斑中发现了磁重联流入的重要证据。耀斑发生在耀斑的东北边缘，呈现出一个漂亮的尖状软X射线环和典型的长时间耀斑的等离子体抛射。对同一耀斑的极紫外光观测显示，我们看到了气泡状的空洞喷发。这个EUV空洞的核心对应于软X射线等离子体。此外，当这个空隙被弹出时，在断开点发生了磁重联。可以看到朝向磁性X点的清晰的持续模式。这一视运动的速度约为5公里S-1，这是重联流入速度的上限。在此基础上，我们推导出重联率为MA=0.001-0.03，其中MA为流入的马赫数。
We found an important piece of evidence for magnetic reconnection inflow in a flare on 1999 March 18. The flare occurred on the northeast limb, displaying a nice cusp-shaped soft X-ray loop and a plasmoid ejection typical for the long-duration events. The EUV observation of the same flare shows us a bubble-like void ejection. The core of this EUV void corresponds to the soft X-ray plasmoid. Moreover, as this void is ejected, magnetic reconnection occurs at the disconnecting point. A clear ongoing pattern toward the magnetic X-point is seen. The velocity of this apparent motion is about 5 km s-1, which is an upper limit on reconnection inflow speed. Based on this observation, we derive the reconnection rate as MA = 0.001-0.03, where MA is an Alfvén Mach number of the inflow.