Solar-Terrestrial Physics Solar-Terrestrial Physics Solar-Terrestrial Physics 2500-0535 29436 10.12737/stp-52201902 14th China-Russia Space Weather Workshop. November 5–9, 2018, Haikou, China 14th China-Russia Space Weather Workshop. November 5–9, 2018, Haikou, China 14th China-Russia Space Weather Workshop. November 5–9, 2018, Haikou, China Alfvén waves in the magnetosphere generated by shock wave/plasmapause interaction Alfvén waves in the magnetosphere generated by shock wave/plasmapause interaction Леонович Анатолий Сергеевич Leonovich Anatoliy Sergeevich leon@iszf.irk.ru

доктор физико-математических наук;

doctor of physical and mathematical sciences;

 Цзун Цюган Zong Qiugang qgzong@pku.edu.cn https://orcid.org/0000-0003-0009-4927 Козлов Даниил Анатольевич Kozlov Daniil Anatolyevich kozlov-da@iszf.irk.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Ван Юнфу Wang Yongfu wyffrank@gmail.com Институт солнечно-земной физики СО РАН Иркутск Россия Institute of Solar Terrestrial Physics SB RAS Irkutsk Russian Federation Институт космической физики и прикладных технологий, Пекинский университет Пекин Китайская Народная Республика Institute of Space Physics and Applied Technology, Peking University Beijing China Институт солнечно-земной физики СО РАН Иркутск Россия Institute of Solar Terrestrial Physics SB RAS Irkutsk Russian Federation Институт космической физики и прикладных технологий, Пекинский университет Пекин Китайская Народная Республика Institute of Space Physics and Applied Technology, Peking University Beijing China 5 2 9 14 https://zh-szf.ru/en/nauka/article/29436/view

We study Alfvén waves generated in the magnetosphere during the passage of an interplanetary shock wave. After shock wave passage, the oscillations with typical Alfvén wave dispersion have been detected in spacecraft observations inside the magnetosphere. The most frequently observed oscillations are those with toroidal polarization; their spatial structure is described well by the field line resonance (FLR) theory. The oscillations with poloidal polarization are observed after shock wave passage as well. They cannot be generated by FLR and cannot result from instability of high-energy particle fluxes because no such fluxes were detected at that time. We discuss an alternative hypothesis suggesting that resonant Alfvén waves are excited by a secondary source: a highly localized pulse of fast magnetosonic waves, which is generated in the shock wave/plasmapause contact region. The spectrum of such a source contains oscillation harmonics capable of exciting both the toroidal and poloidal resonant Alfvén waves.

We study Alfvén waves generated in the magnetosphere during the passage of an interplanetary shock wave. After shock wave passage, the oscillations with typical Alfvén wave dispersion have been detected in spacecraft observations inside the magnetosphere. The most frequently observed oscillations are those with toroidal polarization; their spatial structure is described well by the field line resonance (FLR) theory. The oscillations with poloidal polarization are observed after shock wave passage as well. They cannot be generated by FLR and cannot result from instability of high-energy particle fluxes because no such fluxes were detected at that time. We discuss an alternative hypothesis suggesting that resonant Alfvén waves are excited by a secondary source: a highly localized pulse of fast magnetosonic waves, which is generated in the shock wave/plasmapause contact region. The spectrum of such a source contains oscillation harmonics capable of exciting both the toroidal and poloidal resonant Alfvén waves.

 magnetosphere plasmapause shock front Alfvén waves magnetosphere plasmapause shock front Alfvén waves

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