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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >The Source of Auroral Omegas
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The Source of Auroral Omegas

机译：极光欧米茄的来源

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摘要

The auroral wave-like structures called “omega bands” appear within the post-midnight sector auroral oval with shapes resembling the Greek letter omega, and are typically associated with the recovery phase of substorms. Prior work and MHD simulations suggest both high speed earthward flows and postmidnight flow shears are possible omega band source mechanisms. However, what produces omega bands is not well understood. It is most likely that the paucity of concurrent magnetospheric data has limited our ability to understand fully the mechanism responsible for the generation of the omega bands. We have identified about 263 auroral omegas in seven different THEMIS all sky cameras (ASCs) over a 10 year period. A fraction appear to form from north-south streamers, but some appear to form from east-west auroral arcs. Fifty-one of the 263 Ω also have conjugate or near conjugate THEMIS and GOES spacecraft data. There is evidence in about 80% of these events that high speed earthward flows have occurred prior to or at about the same time as the auroral omega observation. This evidence consists of high speed earthward flows, magnetic field dipolarizations, particle injections into the inner magnetosphere, and auroral streamers. 11 events also show plasma flow data azimuthally along the inner magnetosphere, but for six of these events the V_y component is inconsistent with the auroral omega direction of motion. Of the remaining five events, four have V_y flow shear events but also show evidence of magnetic field dipolarizations, particle injections into the inner magnetosphere, and auroral streamers. Our observations suggest high speed earthward flows are more likely to be the source of auroral omega bands.
机译：极光波结构称为“ω乐队”出现在午夜之后部门极光椭圆形状像希腊信ω,通常是相关的为亚暴的复苏阶段。磁流体动力模拟表明高速向地面流和postmidnight流剪切机是有可能的ω带源机制。生产ω乐队是不清楚。最有可能并发的缺乏磁性层的数据的能力有限充分理解机制ω的生成。识别大约263极光ω在7个不同的忒弥斯所有的天空相机(对asc) 10年时期。南北飘带,但是一些形式从东西方极光弧。Ω也忒弥斯共轭或接近共轭,航天器的数据。大约80%的这些事件,高速度向地球发生之前或在流动大约在同一时间,极光ω观察。dipolarizations向地面流动,磁场,粒子注入内磁层,和极光飘带。沿着内部流动数据方位磁气圈,但六的这些事件与极光V_y组件是不一致的ω的方向运动。事件,四人V_y流剪切事件也dipolarizations表明磁场,粒子注入内磁层,和极光飘带。高速向地面流动更容易极光ω乐队的来源。

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  • 来源
    《Journal of Geophysical Research, A. Space Physics: JGR》 |2022年第1期|2021JA029908-1-2021JA029908-17|共17页
  • 作者

    J. M. Weygand; M. El-Alaoui; H. K. Nykyri;

  • 作者单位

    Institute of Geophysics and Planetary Physics, University of California Los Angeles, Los Angeles, CA, USA;

    NASA Goddard Space Flight Center, Greenbelt, MD, USA;

    Physical Sciences Department College, Daytona College of Arts & Sciences, Embry Riddle Aeronautical University, Daytona Beach, FL, USA;

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