Solar-Terrestrial Physics Solar-Terrestrial Physics Solar-Terrestrial Physics 2500-0535 54806 10.12737/stp-92202304 Results of current research Results of current research Results of current research Differences in the response to CME and CIR drivers of geomagnetic disturbances Differences in the response to CME and CIR drivers of geomagnetic disturbances Намуун Б. Namuun B. Цэгмэд Баттуулай Tsegmed Battuulai tseg@iag.ac.mn

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Ли Л.Ю. Li L.Y. Легари Г.М. Leghari G.M. Школа космонавтики и окружающей среды, Бейханский университет Пекин Китайская Народная Республика School of Space and Environment, Beihang University Beijing China Институт астрономии и геофизики Монгольской академии наук Улан-Батор Монголия Institute of Astronomy and Geophysics, Mongolian Academy of Sciences Ulaanbaatar Mongolia Институт астрономии и геофизики АН Монголии Улан-Батор Монголия Institute of Astronomy and Geophysics AS Mongolia Ulaan-Baatar Mongolia Школа космонавтики и окружающей среды, Бейханский университет Пекин Китайская Народная Республика School of Space and Environment, Beihang University Beijing China Ключевая лаборатория мониторинга космической среды и обработки информации Пекин Китайская Народная Республика Key Laboratory of Space Environment monitoring and Infor-mation Processing of MIIT Beijing China Школа космонавтики и окружающей среды, Бейханский университет Пекин Китайская Народная Республика School of Space and Environment, Beihang University Beijing China Пакистанская комиссия по исследованию космоса и верхних слоев атмосферы Исламабад Пакистан Pakistan Space and Upper Atmosphere Research Commission Islamabad Pakistan 29 06 2023 29 06 2023 9 2 31 36 25 10 2022 10 04 2023 https://naukaru.ru/en/nauka/article/54806/view

Utilizing 1-minute resolution data on the geomagnetic indices SYM-H, AE, solar wind parameters (velocity Vsw and density Np), and z-component Bz of the interplanetary magnetic field (IMF) during solar cycles 23 and 24, we have statistically analyzed the correlations between geomagnetic activity (storms and substorms), Vsw, Np, Bz, and energy coupling functions of solar wind and Earth’s magnetosphere. For the selected 131 CME-driven storms, SYM-H stronger depends on Vsw and B than other parameters, whereas the selected 161 CIR-driven storms have nearly the same dependence on the solar wind electric field, the rate of open magnetic flux dφ/dt, and the reconnection electric field Ekl. Thus, the solar wind electric field and the dayside magnetic reconnection are likely to have different contributions for storms of the two types. During storms of different types, the substorm intensity AE relies mainly on the IMF Bz, rate of open magnetic flux and reconnection electric field.

Utilizing 1-minute resolution data on the geomagnetic indices SYM-H, AE, solar wind parameters (velocity Vsw and density Np), and z-component Bz of the interplanetary magnetic field (IMF) during solar cycles 23 and 24, we have statistically analyzed the correlations between geomagnetic activity (storms and substorms), Vsw, Np, Bz, and energy coupling functions of solar wind and Earth’s magnetosphere. For the selected 131 CME-driven storms, SYM-H stronger depends on Vsw and B than other parameters, whereas the selected 161 CIR-driven storms have nearly the same dependence on the solar wind electric field, the rate of open magnetic flux dφ/dt, and the reconnection electric field Ekl. Thus, the solar wind electric field and the dayside magnetic reconnection are likely to have different contributions for storms of the two types. During storms of different types, the substorm intensity AE relies mainly on the IMF Bz, rate of open magnetic flux and reconnection electric field.

 solar wind coronal mass ejections corotating interaction regions geomagnetic storms magnetospheric substorms correlations solar wind coronal mass ejections corotating interaction regions geomagnetic storms magnetospheric substorms correlations

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