Continuous tailward flow in the near-Earth magnetotail observed by TC-1 satellite  

作　　者：HANG LingQian LIU ZhenXing MA ZhiWei PU ZuYin WANG JiYe SHEN Chao 

机构地区：[1]Center for Space Science and Applied Research, Chinese Academy of Sciences, Beijing 100080, China [2]Institute of Plasma Physics, Chinese Academy of Sciences, Hefei 230031, China [3]School of Earth and Space Science, Peking University, Beijing 100871, China [4]Physics and Electron Engineering Academy, Central Nationality University, Beijing 100081, China

出　　处：《Chinese Science Bulletin》2007年第14期1980-1985,共6页

基　　金：Supported by the National Natural Science Foundation of China (Grant Nos. 40390150, 40474058 and 40125012)

摘　　要：On July 11, 2004, a substorm process in the period of continuous tailward flow was observed by the joint exploration of the TC-1, IMAGE and ACE satellites. The substorm observed by the TC-1 in the near-Earth has three stages: the growth phase (from 11:43 to 12:19), the pre-expansion process (from 12:19 to 12:28) and the dipolarization process. The auroral brightening was at 12:26 recorded by the FUV instrument on IMAGE, and the dipolarization occurred two minutes later. During the 45 min period of the tailward flow, the magnetotail experienced the growth phase and the pre-expansion process. When the dipolarization process began, the TC-1 entered the plasma sheet and observed a high speed earthward flow. The field-aligned tailward flow is characterized by the low temperature and high density, which is consistent with the properties of the flow from the ionosphere detected in the near-Earth magnetotail by other satellites. The tailward flow is closely related with the southward interplanetary magnetic field (IMF), and may have an important effect on the substorm.On July 11, 2004, a substorm process in the period of continuous tailward flow was observed by the joint exploration of the TC-1, IMAGE and ACE satellites. The substorm observed by the TC-1 in the near-Earth has three stages： the growth phase （from 11：43 to 12：19）, the pre-expansion process （from 12：19 to 12：28） and the dipolarization process. The auroral brightening was at 12：26 recorded by the FUV instrument on IMAGE, and the dipolarization occurred two minutes later. During the 45 min period of the tailward flow, the magnetotail experienced the growth phase and the pre-expansion process. When the dipolarization process began, the TC-1 entered the plasma sheet and observed a high speed earthward flow. The field-aligned tailward flow is characterized by the low temperature and high density, which is consistent with the properties of the flow from the ionosphere detected in the near-Earth magnetotail by other satellites. The tailward flow is closely related with the southward interplanetary magnetic field （IMF）, and may have an important effect on the substorm.

关 键 词：风暴 磁层尾 人造卫星 气候 

分 类 号：P46[天文地球—大气科学及气象学]