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Storm-time fingerprints and global profiles of ULF wave power at geosynchronous orbit

机译：地球同步轨道上的ULF波功率的风暴时间指纹和全局轮廓

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摘要

We examine the relationship between long-period (Pc4 and Pc5) ULF wave power and the rapid increase in relativistic electron fluxes observed during some magnetic storms. A qualitative comparison of the ULF dynamic power spectra of the total field magnitude (compressional component) during two major storms indicates a sustained, broadband enhancement of ULF power beginning in the main phase and extending well into the recovery phase for the storm with relativistic electrons. The ULF compressional power increase appears more narrowband and not as sustained during the storm without such electrons. A statistical study using a database of 42 isolated storms indicates that an extended period of elevated Pc5 power throughout the recovery phase may be necessary for electron energization. A similar, albeit weaker effect is observed for Pc4 waves. Finally, the average local-time profiles of Pc4 and Pc5 wave power at geosynchronous orbit are calculated for the early, intermediate, and late stages of the recovery phase for our storm database. A clear difference in the local-time distribution of Pc5 power during the early recovery phase between storms with relativistic electrons and those without is observed. In both cases, there is a Pc5 power peak in the afternoon. However, there are also comparable levels of wave power in the morning sector for storms during which electrons are accelerated to relativistic speeds. This may indicate that high Pc5 power levels occurring on both the dawn and dusk flanks are necessary to "kickstart" the electron acceleration and are one of the factors in differentiating between magnetic storms with enhanced relativistic electron fluxes and those without.
机译：我们检查了长周期（Pc4和Pc5）ULF波功率与在某些磁暴期间观测到的相对论电子通量快速增加之间的关系。在两次大暴风雨中，总场强（压缩分量）的ULF动态功率谱的定性比较表明，从相对论电子开始，ULF功率的持续宽带增强从主阶段开始，一直延伸到风暴的恢复阶段。 ULF压缩功率的增加显得更窄带，并且在没有此类电子的暴风雨期间不会持续。使用42个孤立暴风雨的数据库进行的统计研究表明，在整个恢复阶段，延长的Pc5功率可能需要长时间进行电子激励。对于Pc4波，观察到了类似的效果，但效果较弱。最后，针对风暴数据库的恢复阶段的早期，中间和后期，计算了地球同步轨道上Pc4和Pc5波功率的平均本地时间剖面。在早期恢复阶段，在具有相对论性电子的风暴与没有相对性电子的风暴之间，Pc5功率的本地时间分布存在明显差异。在这两种情况下，下午都有一个Pc5功率峰值。但是，在暴风雨中，电子也被加速到相对论速度，在暴风雨中，波能的水平也相当。这可能表明，在黎明和黄昏时分出现的高Pc5功率水平是“启动”电子加速所必需的，并且是区分具有相对论电子通量的磁暴和不具有相对论电子通量的磁暴的因素之一。

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  • 来源
    《Planetary and space science》 |2009年第15期|p.2087-2094|共8页
  • 作者

    J. Sanny; D. Berube; A. Trevelyan; B. Sorbom; P. Amy;

  • 作者单位

    Physics Department, Loyola Marymount University, I LMU Drive, Los Angeles, CA 90045, USA;

    Physics Department, Loyola Marymount University, I LMU Drive, Los Angeles, CA 90045, USA;

    Physics Department, Loyola Marymount University, I LMU Drive, Los Angeles, CA 90045, USA;

    Physics Department, Loyola Marymount University, I LMU Drive, Los Angeles, CA 90045, USA;

    Physics Department, Loyola Marymount University, I LMU Drive, Los Angeles, CA 90045, USA;

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  • 正文语种 eng
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  • 关键词

    ulf waves; relativistic electrons; geomagnetic storms;

    机译：硫波;相对论电子;地磁风暴;

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