Relativistic electron dynamics in the inner magnetosphere — a review
Relativistic electron dynamics in the inner magnetosphere — a review
复制标题
DOI：
10.1016/s1364-6826(01)00088-8
复制
发表时间：
2002
影响因子：
1.9
通讯作者：
R. Friedel;G. Reeves;T. Obara
中科院分区：
文献类型：
--
作者：
R. Friedel;G. Reeves;T. Obara
近年来，内磁层中相对论性电子在地磁扰动前后的动力学受到了相当大的关注。除了这些电子对MEO和GEO轨道上的空间硬件造成的环境影响，以及它们对空间天气的明显影响外，围绕这些粒子在磁层内部的输运、加速和损失的科学问题还没有完全解决。理解相对论性电子动力学的主要困难之一是它们与地球磁层动力学的主要太阳风驱动因素（太阳风速度、密度和磁场强度/方向）和代表这些动力学的主要指标（Dst、Ae、Kp）之间有些不相关的行为。在地球同步高度观测到的相对论性电子在磁暴发生几天后达到峰值，对于看似相似的地磁干扰/磁暴，可能会出现广泛的响应。本文对相对论电子动力学的研究现状进行了综述和比较，包括简单扩散、亚暴加速、极低频波加速、极低频波再循环或等离子体嘶哑。我们提出了最近一项统计研究的结果，该研究确定了在风暴期间至少持续12小时的足够ULF波能是地球同步高度随后相对论性电子增强的最有效的地球指标。为了完整起见，我们还简要地考察了一些与相对论性电子损失有关的问题和思想。
The dynamics of relativistic electrons in the inner magnetosphere around the time of geomagnetic disturbances have received considerable attention in recent years. In addition to the environmental impact these electrons have on space-hardware in MEO and GEO orbits, and their obvious impact on space weather, the scientific issues surrounding the transport, acceleration and loss of these particles in the inner magnetosphere have not been fully resolved. One of the prime difficulties in understanding the dynamics of relativistic electrons is their somewhat uncorrelated behavior with regard to the major solar wind drivers of the Earth's magnetospheric dynamics (solar wind velocity, density and magnetic field strength/direction) and the major indices representing these dynamics (Dst, Ae, Kp). Relativistic electrons observed at geosynchronous altitude reach their peak several days after the onset of a magnetic storm, and a wide range of responses can occur for seemingly similar geomagnetic disturbances/storms. We give here a review and comparison of the current state of research into relativistic electron dynamics, covering simple diffusion, substorm acceleration, ULF wave acceleration, recirculation by ULF waves or plasmaspheric hiss. We present the results of a recent statistical study which has identified the presence of sufficient ULF wave power for a duration of at least 12 h during a storm as being the most geoeffective indicator of subsequent relativistic electron enhancements at geosynchronous altitudes. For completeness we also briefly examine some of the problems and ideas related to relativistic electron losses.