Inner belt and slot region electron lifetimes and energization rates based on AKEBONO statistics of whistler waves
Inner belt and slot region electron lifetimes and energization rates based on AKEBONO statistics of whistler waves
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DOI：
10.1002/2014ja019886
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发表时间：
2014-04
期刊：
影响因子：
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通讯作者：
O. Agapitov;A. Artemyev;D. Mourenas;Y. Kasahara;V. Krasnoselskikh
中科院分区：
文献类型：
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作者：
O. Agapitov;A. Artemyev;D. Mourenas;Y. Kasahara;V. Krasnoselskikh
从EXOS-D(Akebono)卫星上获得了来自地面甚低频发射机的嘶鸣、闪电和其他哨声模波的全球统计数据，并将其拟合为两个地磁活动范围(Kp3)的L和纬度的函数。特别是，本研究集中在内带L∈[1.4，2]，在那里缺乏可靠的现场测量。这些统计数据对于准确评估每种波在内辐射带动态中的作用和相对优势是至关重要的。而在L，甚低频波似乎主要以导管模式传播)，∼为1.5-3)。希斯波通常在内带最强烈，闪电和嘶嘶波的强度随着地磁活动的增加而增加。在Kp和lt；2磁声波振幅较弱的L和lt；2区，闪电产生的波幅一般在赤道10°以内达到峰值。在此基础上，给出了每种波型的简化模型。然后用全波模型计算了电子的准线性螺距角和能量扩散率。相应的电子寿命与L∈[1.4，2]上太阳反常粒子探测器和磁层粒子探测器和其他卫星获得的俘获高能电子的衰减率相当。
Global statistics of the amplitude distributions of hiss, lightning‐generated, and other whistler mode waves from terrestrial VLF transmitters have been obtained from the EXOS‐D (Akebono) satellite in the Earth's plasmasphere and fitted as functions of L and latitude for two geomagnetic activity ranges (Kp3). In particular, the present study focuses on the inner zone L∈[1.4,2] where reliable in situ measurements were lacking. Such statistics are critically needed for an accurate assessment of the role and relative dominance of each type of wave in the dynamics of the inner radiation belt. While VLF waves seem to propagate mainly in a ducted mode at L∼1.5–3 for Kp3). Hiss waves are generally the most intense in the inner belt, and lightning‐generated and hiss wave intensities increase with geomagnetic activity. Lightning‐generated wave amplitudes generally peak within 10° of the equator in the region L<2 where magnetosonic wave amplitudes are weak for Kp<3. Based on this statistics, simplified models of each wave type are presented. Quasi‐linear pitch angle and energy diffusion rates of electrons by the full wave model are then calculated. Corresponding electron lifetimes compare well with decay rates of trapped energetic electrons obtained from Solar Anomalous and Magnetospheric Particle Explorer and other satellites at L∈[1.4,2].