Impact of Geomagnetic Storms on L-band Ionospheric Scintillation Over Equatorial Region
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摘要: 利用赤道地区Vamimo站闪烁数据, 选取两次典型大磁暴时段重点分析, 对比磁暴发生前、发生时以及发生后连续几天电离层幅度闪烁强度和发生率的变化, 引入瑞利elax-elax泰勒不稳定性(Rayleigh-Taylor, R-T不稳定性)线性增长率γ0, 对磁暴影响闪烁的机制进行初步探讨. 结果表明, 磁暴可能触发闪烁发生, 也可能抑制闪烁发生, 这既与观测季节有关, 也与磁暴不同发展阶段的地方时有关. 触发发生于闪烁少发季节磁暴主相所在的午夜至黎明时段, 可能是磁层穿透电离层的东向电场所致; 抑制发生于闪烁多发季节磁暴恢复相所在的午夜前时段, 可能是西向电场作用的结果. 磁暴发生时的电场变化可能是抑制或触发闪烁的主导因素, 但仍需进一步分析研究.Abstract: Using the observation data at Vanimo station, the amplitude scintillation intensity and the occurrence rate were analyzed during the two classic different strong magnetic storms. Mechanism of the magnetic storm influence on the scintillation was discussed preliminarily by Rayleigh-Taylor instability linear theory. The results show that the magnetic storm could either triggering or inhibiting the scintillation, which relates to the season and the local time of the different period of the magnetic storm. If the magnetic storm main phase occurs from midnight to dawn, the scintillation may be triggered by the eastern ward electrical field, and if the magnetic storm recovery phase takes place during the pre-midnight, it may be inhibited by the western ward electrical field. The electrical field variation during the magnetic storms is possibly the main factor that influence the scintillation, but it needs further study to prove.
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