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THEMIS双卫星对磁尾高速流减速的联合观测 被引量:3
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作者 商文赛 尧中华 +7 位作者 史全岐 孙为杰 傅绥燕 刘江 田安民 宗秋刚 濮祖荫 肖婷 《科学通报》 EI CAS CSCD 北大核心 2014年第3期297-305,共9页
磁尾等离子体片高速流的运动和减速过程对于磁层粒子的加速、磁场的扰动、磁通量的输运和亚暴的触发以及磁尾电流系统的形成都具有重要意义。2009年2~4月,THEMIS卫星中的2颗星(THA和THE)在空间中经常具有相近的XGSM和YGSM坐标,但具... 磁尾等离子体片高速流的运动和减速过程对于磁层粒子的加速、磁场的扰动、磁通量的输运和亚暴的触发以及磁尾电流系统的形成都具有重要意义。2009年2~4月,THEMIS卫星中的2颗星(THA和THE)在空间中经常具有相近的XGSM和YGSM坐标,但具有差别较大的ZGSM坐标。我们利用这种特殊构型的2颗卫星对经过等离子体片中心和边界层附近的高速流进行了联合观测研究。通过个例和统计分析发现,在89%的地向高速流事件中,距离中性片较远的卫星先观测到高速流,其速度以平行于磁场的分量为主,并且95%的事件中距离中性片较远的卫星所探测到高速流X分量的速度最大值要比在片中心探测到的高速流数值更大。假设等离子体片边界层附近的平行高速流匀速传播,而对于中心等离子体片的高速流,我们分别应用匀减速模型与突然减速模型进行分析,发现高速流减速起始的位置大部分位于距离地球15 Re的区域,这与中磁尾重联发生区域比较接近。此外,统计结果表明等离子体片中心高速流前端往往伴随着明显的偶极化锋面特征,而远离中性片的地方偶极化锋面的特征则不明显。 展开更多
关键词 高速流 等离子体片 偶极化锋面 磁场重联 亚暴
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地球磁尾不同位置处高速流的统计特性研究 被引量:1
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作者 潘东晓 孙为杰 +6 位作者 史全岐 田安民 YAO ZhongHua 傅绥燕 宗秋刚 周煦之 濮祖荫 《中国科学:地球科学》 CSCD 北大核心 2015年第12期1866-1874,共9页
使用2007~2011年THEMIS卫星数据,对位于地球磁尾(|YGSM|〈13RE,|ZGSM|〈5RE。
关键词 磁尾高速流 地向演化 行星际磁场
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Braking of high-speed flows in the magnetotail:THEMIS joint observations 被引量:3
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作者 Wensai Shang Zhonghua Yao +8 位作者 Quanqi Shi Weijie Sun Suiyan Fu Jiang Liu Anmin Tian Qiugang Zong Zuyin Pu Ting Xiao Vassilis Angelopoulos 《Chinese Science Bulletin》 SCIE EI CAS 2014年第3期326-334,共9页
The motion and deceleration processes of plasma sheet high-speed flows have great significance to magnetospheric particle acceleration,magnetic field perturbation,magnetic flux transport,triggering of substorm,and the... The motion and deceleration processes of plasma sheet high-speed flows have great significance to magnetospheric particle acceleration,magnetic field perturbation,magnetic flux transport,triggering of substorm,and the current system formation in the magnetotail.From February to April 2009,two satellites of the Time History of Events and Macroscale Interactions during Substorms mission,THA and THE,were often separated largely in Z direction,but had small X and Y separations.Such special configuration allows simultaneous observations of highspeed flows at the center and boundary of the plasma sheet.Based on selected case study and statistical analysis,it is found that for about 89%of the events we selected,the probe further away from the neutral sheet observed the high-speed flow earlier than the one close to the center,and the flow is mainly field aligned.And for about 95%events the probe further away from the neutral sheet observed higher X component of the plasma flow.With the hypothesis that parallel flow keeps the same speed during its earthward propagation while central plasma sheet stream uniformly or suddenly brakes on its way to the earth,we deduced the position where the deceleration begins to be between 13 Re and 17 Re downtail,where thenear-earth reconnection is supposed to occur.In addition,our statistical results show that dipolarization fronts observed in the central plasma sheet are more prominent than those observed in the plasma sheet boundary layer ahead of the high-speed flow. 展开更多
关键词 高速制动 观测 等离子体片 磁流 减速过程 统计分析 边界层流 等离子体流
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THEMIS statistical study on the plasma properties of high-speed flows in Earth's magnetotail 被引量:2
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作者 PAN Dong Xiao SUN Wei Jie +6 位作者 SHI Quan Qi TIAN An Min YAO Zhong Hua FU Sui Yan ZONG Qiu Gang ZHOU Xu Zhi PU Zu Yin 《Science China Earth Sciences》 SCIE EI CAS CSCD 2016年第3期548-555,共8页
Using Time History of Events and Macroscale Interactions during Substorms (THEMIS) observations from 2007 to 2011 tail seasons, we study the plasma properties of high speed flows (HSFs) and background plasma sheet... Using Time History of Events and Macroscale Interactions during Substorms (THEMIS) observations from 2007 to 2011 tail seasons, we study the plasma properties of high speed flows (HSFs) and background plasma sheet events (BPSs) in Earth's magnetotail (|YGsM|〈13RE, |ZGsM|〈5RE, -30RE〈XrsM〈-6RE), and their correlations with solar wind parameters. Statistical results show that the closer the HSFs and BPSs are to the Earth, the hotter they become, and the temperature increase of HSFs is larger than that of BPSs. The density and temperature ratios between HSFs and BPSs are also larger when events are closer to Earth. We also find that the best correlations between the HSFs (BPSs) density and the solar wind density occur when the solar wind density is averaged 2 (3.5) hours prior to the onset of HSFs (BPSs). The normalized densities of both HSFs and BPSs are correlated with the interplanetary magnetic field (IMF) 0 angles ( 0 = arctan(Bz √Bx^2+y^2 ) which are averaged 3 hours before the observation time. Further analysis indicates that both HSFs and BPSs become denser during the northward IMF period. 展开更多
关键词 High-speed flow Earthward evolution Interplanetary magnetic field
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