Energetic electrons associated with magnetic reconnection in the sheath of interplanetary coronal mass ejection  

作　　者：HUANG ShiYong DENG XiaoHua ZHOU Meng YUAN ZhiGang LI HuiMin WANG DeDong 

机构地区：[1]School of Electronic Information, Wuhan University, Wuhan 430072, China [2]State Key Laboratory of Space Weather, Chinese Academy of Sciences, Beijing 100190, China [3]Institute of Space Science and Technology, Nanchang University, Nanchang 330031, China

出　　处：《Chinese Science Bulletin》2012年第12期1455-1460,共6页

基　　金：supported by the National Natural Science Foundation of China(40890163);the Fundamental Research Funds for the Central Universities;the Specialized Research Fund for State Key Laboratories,Chinese Academy of Sciences

摘　　要：Magnetic reconnection is an important universal plasma dissipation process that converts magnetic energy into plasma thermal and kinetic energy,and simultaneously changes the magnetic field topology.In this paper,we report the first observation of energetic electrons associated with asymmetric reconnection in the sheath of an interplanetary coronal mass ejection.The magnetic field shear angle was about 151°,implying guide-field reconnection.The width of the exhaust was about 8×104 km.The reconnection rate was estimated as 0.044-0.08,which is consistent with fast reconnection theory and previous observations.We observed flux enhancements of energetic electrons with energy up to 400 keV in this reconnection exhaust.The region where ener- getic electron fluxes were enhanced is located at one pair of separatrices in the higher density hemisphere.We discuss these observation results,and compare with previous observations and recent kinetic simulations.Magnetic reconnection is an important universal plasma dissipation process that converts magnetic energy into plasma thermal and kinetic energy, and simultaneously changes the magnetic field topology. In this paper, we report the first observation of ener- getic electrons associated with asymmetric reconnection in the sheath of an interplanetary coronal mass ejection. The magnetic field shear angle was about 151°, implying guide-field reconnection. The width of the exhaust was about 8x104 km. The recon- nection rate was estimated as 0.044-0.08, which is consistent with fast reconnection theory and previous observations. We ob- served flux enhancements of energetic electrons with energy up to 400 keV in this reconnection exhaust. The region where ener- getic electron fluxes were enhanced is located at one pair of separatrices in the higher density hemisphere, We discuss these ob- servation results, and compare with previous observations and recent kinetic simulations.

关 键 词：日冕物质抛射 高能电子 磁重联 行星际 动力学模拟 等离子体 动能转换 耗散过程 

分 类 号：P353.7[天文地球—空间物理学]