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摘要
We build empirical models of magnetosonic waves (also called as equatorial noise) both outside and inside the plasmapause, based on the Time History of Events and Macroscale Interactions during Substorms fast-survey data during the period from 1 May 2010 to 30 November 2014, which utilize solar wind measurements as model inputs, i.e., interplanetary magnetic field (IMF) B-z, solar wind speed (V-SW), and dynamic pressure (P-SW). For model development, the time delay of magnetosonic wave amplitude relative to the solar wind parameters is first identified based on correlation analysis. We find that P-SW is better correlated with the variation of wave amplitude outside the plasmapause than V-SW, while the opposite is true inside the plasmapause. Among the solar wind parameters, the preceding southward IMF B-z with the time delay of 3-4h and 4-5h, corresponding to outside and inside the plasmapause, respectively, yields the best correlation with the variation of wave amplitude. In this study, we use the solar wind parameter-based model to investigate magnetosonic wave activity during corotating interaction region-driven storm. The results show that with increasing southward IMF B-z, wave activity is amplified mostly on the dayside both outside and inside the plasmapause and high amplitude is more shifted toward the prenoon sector, while increasing P-SW, it is amplified only in the postnoon sector outside the plasmapause. Our statistical model can explain the observed amplitudes by 38% on average outside the plasmapause and 26% inside, and their model performance is generally higher than that of a model using AE index only as an input.
- 出版日期2016-1
