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Small- and Middle-scale Solar Wind Structures, Transferringfrom Solar Wind to the Magnetosheath: Correlation Analysisстатья
- Авторы: Rakhmanova L.S., Riazantseva M.O., Zastenker G.N.
- Сборник: WDS'13 Proceedings of Contributed Papers: Part II – Physics of Plasmas and Ionized (eds. J. Safrankova and J. Pavlu)
- Год издания: 2013
- Место издания: Matfyzpress Prague
- Первая страница: 30
- Последняя страница: 36
- Аннотация: The paper is based on the correlation analysis of small- and middle-scale plasma structures of solar wind (SW) and their evolution during propagation through the bow shock (BS) to the magnetosheath (MSH). We have used data obtained from two closely located THEMIS satellites upstream and downstream from the BS. We obtain the correlation coefficient as function of UT and the time lag between SW and MSH data. Correlation coefficient is calculated for the primary data and for smoothed data. Smoothing time ranges from 10 to 170 seconds. We consider the dependence of correlation coefficient on smoothing time. We have found that correlation coefficient doesn’t significantly depend on smoothing time for data with smoothing time exceeded 50 seconds. This means that BS and MSH add to the solar wind plasma density fluctuations predominantly high-frequency variations with frequencies exceeded 0.02 Hz. We also consider continuous 20-hour interval of plasma density measurements and time evolution of correlation coefficient during that interval. We find that correlations can decrease to insignificant values in several minutes and then increase again. It was shown that sharp changes of correlation coefficient are associated with changes of different parameters: QBn angle, the distance between spacecraft along Ygse axis and on interplanetary magnetic field (IMF) rotation.
- Добавил в систему: Рязанцева Мария Олеговна