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Dayside poleward moving auroral forms and ionospheric convection under stable interplanetary magnetic field (IMF) conditions

查看全文 作　　者：XING [1,2]ZanYang;YANG [2]HuiGen;HAN [2]DeSheng;WU [1]ZhenSen;LIU [2]JunMing;HU [2]ZeJun;ZHANG [2]QingHe;HU [2]HongQiao;LIU [2]YongHua 高影响力作者 机构地区：[1]School of Science,Xidian University;[2]SOA Key Laboratory for Polar Science,Polar Research Institute of China高影响力机构 出　　处：《Science China(Technological Sciences)》索引2013年第56卷第4期,共7页高影响力期刊 基　　金：supported by the National Natural Science Foundation of China (Grant Nos. 41031064,40974103,40974083,40904041,40890164,41104091,and 41104090);the Polar Strategic Research Foundation of China (Grant No. 20120304);the Ocean Public Welfare Scientific Research Project,State Oceanic Administration of the People's Republic of China (Grant No. 201005017) 摘　　要：Using high temporal resolution optical data obtained from three-wavelength all-sky imagers over six winters continuously at Yellow River Station (78.92°N,11.93°E) in Arctic,we statistically investigated the dependence of location of poleward moving auroral forms (PMAFs) on the interplanetary magnetic field (IMF) B z and B y components as a function of MLT and MLAT under stable IMF conditions.It is found that more PMAFs occurred in lower latitude for Bz<0 and there was less evident IMF B y-related prenoon-postnoon asymmetry for Bz<0 than for Bz>0.We found that the PMAFs were distributed over a wide range of MLT when Bz<0,which indicates that the reconnection X-line might spread like an 'S' shape.However,during northward IMF,PMAFs were observed predominantly prenoon for IMF By>0 and postnoon for IMF By<0 associating with the effect of the high-latitude reconnection,which is largely consistent with the theoretical model of the convection flow. 关 键 词：行星际磁场 稳定条件 IMF 移动 极地 极光 电离层 国际货币基金组织
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