论文部分内容阅读
当行星际磁场持续南向时,磁尾尾瓣区积蓄大量的磁能,出现强的晨昏电场.此时中磁尾磁重联进行得深入持久,在等离子体片闭合磁场和等离子体被带出重联区之后,尾瓣区的磁场和等离子体不断进入重联区,这种重联过程称之为“持续尾瓣重联”(CLR).分析2001~2003年期间欧空局Cluster星簇对中磁尾的观测数据,发现CLR除导致磁场形态改变和产生高速流外,重联区出现空泡,多数空泡中等离子体密度和温度下降两个数量级(少数为一个数量级).空泡结束后,密度较重联前低,温度略有升高.CLR的持续时间一般为几十分钟,它同行星际磁场持续南向发生的强亚暴有很好的相关性.
When the interplanetary magnetic field continues to the south, the tail-tail region accumulates a large amount of magnetic energy, resulting in a strong dusk electric field. At this time, the magnetic tail-magnetic reconnection proceeds deeply and permanently. After the plasma slice closes the magnetic field and the plasma is taken out of the weight After the zone, the magnetic fields and plasma in the tail-valve zone continue to enter the reconnection zone, and this reconnection process is called “persistent tail flap reconnection” (CLR). Analysis of the ESA cluster star clusters during 2001-2003 In the middle magnet tail observation data, it was found that in addition to the change of magnetic field shape and the high velocity flow generated by CLR, cavitation occurs in the reconnection zone, and the plasma density and temperature in most cavities decrease by two orders of magnitude (a few orders of magnitude) After the density is low, the temperature is slightly higher, and the duration of the CLR is usually several tens of minutes, which has a good correlation with the strong sub-storms that occur in the south of the interplanetary magnetic field.