ELF/VLF wave propagation at subauroral latitudes: Conjugate observation between the ground and Van Allen Probes A
ELF/VLF wave propagation at subauroral latitudes: Conjugate observation between the ground and Van Allen Probes A
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ELF/VLF 波在亚极光纬度的传播：地面和范艾伦探测器 A 之间的共轭观测
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发表时间：
2016
期刊：
影响因子：
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通讯作者：
W. Kurth
中科院分区：
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作者：
C. Martinez‐Calderon;K. Shiokawa;Y. Miyoshi;K. Keika;M. Ozaki;I. Schofield;M. Connors;C. Kletzing;M. Hanzelka;O. Santolík;W. Kurth
我们报告同时观测ELF/VLF的排放，表现出类似的频谱和频率的功能，在Athabasca（ATH），加拿大，（L = 4.3）和货车艾伦探测器A（辐射带风暴探测器（RBSP）A）之间的VLF接收器。我们利用2012年11月1日至2013年10月31日的统计数据库，将地面观测到的总共347次排放与RBSP在磁层的观测进行了比较。2013年2月25日，从12：46到13：39 UT在黎明扇区（04-06磁当地时间（MLT）），我们观察到一个准周期（QP）发射中心在4 kHz，并伴随着短脉冲持续不到一秒的4.8 kHz在黎明扇区（04-06 MLT）。RBSP A波数据显示，这两种发射都是右手极化的，其坡印亭矢量向地球指向北方半球。利用互相关分析，我们首次对地面和空间之间的共轭ELF/VLF事件进行了时间延迟分析，发现QP的时间延迟为+2至+4 s（ATH优先），脉冲的时间延迟为-3 s（RBSP A优先）。利用从ATH到地磁赤道的反向追踪和从赤道到RBSP A的正向追踪，基于航天器观测到的等离子体层密度，我们验证了QP发射的可能传播路径，该路径与观测到的时间延迟一致。
We report simultaneous observation of ELF/VLF emissions, showing similar spectral and frequency features, between a VLF receiver at Athabasca (ATH), Canada, (L = 4.3) and Van Allen Probes A (Radiation Belt Storm Probes (RBSP) A). Using a statistical database from 1 November 2012 to 31 October 2013, we compared a total of 347 emissions observed on the ground with observations made by RBSP in the magnetosphere. On 25 February 2013, from 12:46 to 13:39 UT in the dawn sector (04–06 magnetic local time (MLT)), we observed a quasiperiodic (QP) emission centered at 4 kHz, and an accompanying short pulse lasting less than a second at 4.8 kHz in the dawn sector (04–06 MLT). RBSP A wave data showed both emissions as right‐hand polarized with their Poynting vector earthward to the Northern Hemisphere. Using cross‐correlation analysis, we did, for the first time, time delay analysis of a conjugate ELF/VLF event between ground and space, finding +2 to +4 s (ATH first) for the QP and −3 s (RBSP A first) for the pulse. Using backward tracing from ATH to the geomagnetic equator and forward tracing from the equator to RBSP A, based on plasmaspheric density observed by the spacecraft, we validate a possible propagation path for the QP emission which is consistent with the observed time delay.