THEMIS statistical study on the plasma properties of high-speed flows in Earth＇s magnetotail

作     者：PAN Dong Xiao SUN Wei Jie SHI Quan Qi TIAN An Min YAO Zhong Hua FU Sui Yan ZONG Qiu Gang ZHOU Xu Zhi PU Zu Yin 

作者机构：Shandong Provincial Key Laboratory of Optical Astronomy and Solar Terrestrial Environment School of Space Science and Physics Shandong University Weihai 264209 China State Key Laboratory of Space Weather Chinese Academy of Sciences Beijing 100190 China School of Earth and Space Sciences Peking University Beijing 100871 China Mullard Space Science Laboratory UCL Dorking RH5 6NT UK IGPP/ESS University of California Los Angeles CA 90095-1567 USA 

出 版 物：《Science China Earth Sciences》 (中国科学（地球科学英文版）)

年 卷 期：2016年第59卷第3期

页      面：548-555页

核心收录：

学科分类：07[理学] 070802[理学-空间物理学] 08[工学] 0708[理学-地球物理学] 0827[工学-核科学与技术] 082701[工学-核能科学与工程] 0704[理学-天文学] 

基　　金：National Natural Science Foundation of China (Grant Nos. 41322031, 41031065 & 41574157) the Shandong Province Outstanding Young Scientist Award (Grant No. 2013BSE27132) the Research Fund for the Doctoral Program of Higher Education (Grant No. 20130131120073) the program for New Century Excellent Talents in University (Grant No. NCET-12-0332) State Key Laboratories of Space Weather 

主　　题：等离子体特性 地球磁尾 高速流动 统计 转录因子 Boss 使用事件 温度升高 

摘      要：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(|Y_(GSM)|13R_E, |Z_(GSM)|5R_E, –30R_EX_(GSM)–6R_E), 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) θ angles(θ=arctan(B_Z/((B_x^2)+(B_y^2))^(1/2) which are averaged 3 hours before the observation time. Further analysis indicates that both HSFs and BPSs become denser during the northward IMF period.