Physical Processes of Meso-Scale, Dynamic Auroral Forms
Physical Processes of Meso-Scale, Dynamic Auroral Forms
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DOI：
10.1007/s11214-020-00665-y
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发表时间：
2020-04
影响因子：
10.3
通讯作者：
C. Forsyth;V. Sergeev;M. Henderson;Y. Nishimura;B. Gallardo‐Lacourt
中科院分区：
文献类型：
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作者：
C. Forsyth;V. Sergeev;M. Henderson;Y. Nishimura;B. Gallardo‐Lacourt
中尺度极光形式，如向极边界增强、流光、欧米茄带、珠子和巨大起伏，是磁层动力过程的表现，在很大程度上是由磁尾等离子体不稳定性驱动的。地面和空间仪器的新观测和理论处理使我们对这些极光形式背后的一些物理过程有了更清楚的了解。然而，问题仍然是如何解释这些意见，在映射极光的特点，在磁层的位置的不确定性，并由于从不同的等离子体不稳定性的各种模型的结果显着重叠。我们提供了该领域最新结果的概述，并试图澄清一些关于驱动一些最大和最具活力的极光形式的剩余问题。
Meso-scale auroral forms, such as poleward boundary intensifications, streamers, omega bands, beads and giant undulations, are manifestations of dynamic processes in the magnetosphere driven, to a large part, by plasma instabilities in the magnetotail. New observations from ground- and space-based instrumentation and theoretical treatments are giving us a clearer view of some of the physical processes behind these auroral forms. However, questions remain as to how some of these observations should be interpreted, given uncertainties in mapping auroral features to locations in the magnetotatil and due to the significant overlap in the results from a variety of models of different plasma instabilities. We provide an overview of recent results in the field and seek to clarify some of the remaining questions with regards to what drives some of the largest and most dynamic auroral forms.