Location of Magnetic Reconnection in the Magnetotail
Location of Magnetic Reconnection in the Magnetotail
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DOI：
10.1007/s11214-006-6216-4
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发表时间：
2006-02
影响因子：
10.3
通讯作者：
T. Nagai
中科院分区：
文献类型：
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作者：
T. Nagai
了解亚暴发生时近地磁尾的磁场重联位置是一个至关重要的问题。通过对磁尾的观测发现，控制磁尾磁场重联位置的因素是太阳风能量输入。在高（低）太阳风能量输入条件下，磁重联在磁尾靠近（远离）地球的位置形成。根据早期Vela航天器的观测，人们认为磁重联开始于Vela位置内部，可能在15 RE。后来的ISEE/SEM 2000观测将磁重联的范围扩大到20 RE以上。Vela事件研究是在高度活跃的条件下进行的，而ISEE/ESTA调查研究是在中度或安静的条件下进行的。控制磁尾磁场重联位置的因子的发现，解决了不同航天器观测结果之间的明显差异，揭示了磁尾磁场重联位置的太阳周期变化。
It is a crucial issue to know where magnetic reconnection takes place in the near-Earth magnetotail for substorm onsets. It is found on the basis of Geotail observations that the factor that controls the magnetic reconnection site in the magnetotail is the solar wind energy input. Magnetic reconnection forms close to (far from) the Earth in the magnetotail for high (low) solar wind energy input conditions.With the early Vela spacecraft observations, it was believed that magnetic reconnection started inside the Vela position, likely at 15 RE. The later ISEE/IRM observations put magnetic reconnection beyond 20 RE. The Vela event studies were made for highly active conditions, while the ISEE/IRM survey studies were made for moderate or quiet conditions. The finding of the factor that controls the site of magnetic reconnection in the magnetotail resolves the apparent discrepancy among various spacecraft results, and suggests solar cycle variation of the magnetotail reconnection site.