Energetic electrons in the magnetotail at 60RE
Energetic electrons in the magnetotail at 60RE
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60RE 磁尾中的高能电子
DOI：
10.1029/ja076i004p00862
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发表时间：
1971
影响因子：
--
通讯作者：
C. Meng
中科院分区：
文献类型：
--
作者：
C. Meng
本文介绍了探测器35号卫星在15个磁尾交叉点上对Ee>22 kev和Ee>45 kev的高能电子的观测结果。在两种不同的通量强度（低通量和高通量（截止J（Ee> 22 kev）> 345电子/cm 2秒ster））下示出了纵向和横向分布。在计数率阈值高于宇宙线本底的低通量下，高能电子的出现频率从尾的黎明侧到黄昏侧几乎是相同的。纬向分布表明，高能电子的出现频率在太阳磁层赤道附近最高，离开赤道平面后逐渐下降。在高通量水平（J（Ee> 22 kev）> 345电子/cm ~ 2秒ster和J（Ee> 45 kev）> 278电子/cm ~ 2秒ster），分布强烈依赖于经度和纬度。在黎明侧和赤道附近出现的频率要高得多。通量最少的区域是在黄昏侧的尾部的北方部分。这种黎明到黄昏的不对称性似乎随着通量阈值水平的增加而增加。
Energetic electron (Ee>22 kev and Ee>45 kev) observations of the lunar orbiting Explorer 35 satellite from 15 magnetotail crossings at geocentric distances of about 60RE are presented. The longitudinal and latitudinal distributions are shown at two different flux intensities (low fluxes and high fluxes (cutoff J(Ee>22kev) > 345 electrons/cm2 sec ster)). At low fluxes with the counting rate threshold above the cosmic ray background, the occurrence frequency of energetic electrons is almost the same from the dawn side to the dusk side of the tail. The latitudinal distribution shows the occurrence frequency of energetic electrons to be highest near the solar magnetospheric equator and gradual falling off away from the equatorial plane. At high flux levels (J(Ee>22kev) > 345 electrons/cm2 sec ster and J(Ee>45kev) > 278 electrons/cm2 sec ster), the distributions are strongly dependent on longitude and latitude. The occurrence frequency is much higher in the dawn side and near the equator. The region where fluxes were found least frequently is in the northern part of the tail on the dusk side. This dawn to dusk asymmetry appears to increase with increasing flux threshold levels.