...
  • 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Transport Path of Cold-Dense Plasmas in the Dusk Magnetotail Plasma Sheet: MMS Observations
【24h】

Transport Path of Cold-Dense Plasmas in the Dusk Magnetotail Plasma Sheet: MMS Observations

机译：低温高密度等离子体传输路径的黄昏磁尾等离子体片:MMS的观察

获取原文
获取原文并翻译 | 示例
           
页面导航
  • 摘要
  • 著录项
  • 相似文献
  • 相关主题

摘要

The near-Earth plasma sheet becomes cold and dense under northward interplanetary magnetic field (IMF) condition, which suggests efficient solar wind plasma entry into the magnetosphere across the magnetopause for northward IMF and a possible contribution of ionospheric oxygen ion outflow. The cold and dense characteristics of the plasma sheet are more evident in the magnetotail flank regions that are the interface between cold solar wind plasma and hot magnetospheric plasma. Several physical mechanisms have been proposed to explain the solar wind plasma entry across the magnetopause and resultant formation of the cold-dense plasma sheet (CDPS) in the tail flank regions. However, the transport path of the cold-dense plasma inside the magnetotail has not been understood yet. Here, we present a case study of the CDPS in the dusk magnetotail by magnetospheric multiscale (MMS) spacecraft under strongly northward IMF and high-density solar wind conditions. The ion distribution function consists of high- and low-energy components, and the low-energy one intermittently shows energy dispersion in the directions parallel and antiparallel to the local magnetic field. The time-of-flight analysis of the energy-dispersed low-energy ions suggests that these ions originate in the region farther down the tail, move along the magnetic field toward the ionosphere and then come back to the magnetotail by the mirror reflection. The pitch-angle dispersion analysis gives consistent results on the traveling time and path length of the energy-dispersed ions. Based on these observations, we discuss possible generation mechanisms of the energy-dispersed structure of the low-energy ions during the northward IMF.
机译：近地等离子表变得寒冷和密度在北行星际磁场(IMF)条件,这表明高效的太阳能风等离子体进入磁层磁北国际货币基金组织(IMF)和一个可能的电离层氧离子外流的贡献。寒冷和稠密等离子体的特性在磁尾侧面板更明显区域冷太阳能之间的接口风等离子体和磁性层的热等离子体。提出了几个物理机制在解释太阳风等离子体条目磁层和合成的形成低温高密度等离子体片(cdp)尾部侧面地区。低温高密度等离子体在磁尾没有被理解。在黄昏磁尾cdp的研究磁性层的多尺度(MMS)航天器强烈向北国际货币基金组织(IMF)和高密度的太阳能风条件。由高和低能耗的组件和低能的间歇性地显示了能量在方向平行和色散反平行的当地磁场。飞行时间energy-dispersed的分析低能离子表明这些离子发源于青藏高原沿尾部,沿着磁场向电离层然后回到磁尾镜面反射。色散分析给出了一致的结果旅游的时间和路径长度energy-dispersed离子。观察,我们将讨论可能的一代energy-dispersed结构的机制低能离子在IMF向北。

著录项

相似文献

  • 外文文献
  • 中文文献
获取原文

客服邮箱：kefu@zhangqiaokeyan.com

京公网安备：11010802029741号 ICP备案号：京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有

  • 客服微信

  • 服务号