Solar-Terrestrial Physics Solar-Terrestrial Physics Solar-Terrestrial Physics 2500-0535 49077 10.12737/stp-82202212 17th Annual Conference “Plasma Physics in the Solar System”. February 7–11, 2022, Space Research Institute RAS, Moscow, Russia 17th Annual Conference “Plasma Physics in the Solar System”. February 7–11, 2022, Space Research Institute RAS, Moscow, Russia 17th Annual Conference “Plasma Physics in the Solar System”. February 7–11, 2022, Space Research Institute RAS, Moscow, Russia Geomagnetic pulsations in 1–4 mHz frequency range (Pc5/Pi3) in the magnetotail at different levels of disturbances in the interplanetary medium Geomagnetic pulsations in 1–4 mHz frequency range (Pc5/Pi3) in the magnetotail at different levels of disturbances in the interplanetary medium https://orcid.org/0000-0003-0678-8743 Ягова Надежда Викторовна Yagova Nadezda Viktorovna nyagova@ifz.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 https://orcid.org/0000-0003-0825-151X Козырева Ольга Васильевна Kozyreva Olga Vasilyevna kozyreva@ifz.ru

доктор физико-математических наук;

doctor of physical and mathematical sciences;

 Носикова Наталия Сергеевна Nosikova Nataliya Sergeevna natanosik@yandex.ru Институт физики Земли им. О.Ю. Шмидта РАН Москва Россия Schmidt Institute of Physics of the Earth RAS Moscow Russian Federation Геофизический центр РАН Москва Россия Geophysical Center of the Russian Academy of Sciences Moscow Russian Federation Институт физики Земли им. О.Ю. Шмидта РАН Москва Россия Schmidt Institute of Physics of the Earth, RAS Moscow Russian Federation Институт физики Земли им. О.Ю. Шмидта РАН Москва Россия Schmidt Institute of Physics of the Earth, RAS Moscow Russian Federation Национальный исследовательский ядерный университет «МИФИ» Москва Россия National Research Nuclear University “MEPhI” Moscow Russian Federation 30 06 2022 30 06 2022 8 2 76 83 03 03 2022 16 05 2022 https://naukaru.ru/en/nauka/article/49077/view

In this paper, we study parameters of geomagnetic pulsations in the 1–4 mHz frequency range (Pc5/Pi3) in the magnetotail, utilizing data obtained by Cluster satellites at different levels of fluctuations in the interplanetary magnetic field (IMF) and the solar wind dynamic pressure in 2016. Particular attention is given to the conditions of “zero” disturbance when amplitudes of fluctuations in the interplanetary medium are smaller compared to their typical values. Both under quiet and disturbed conditions, waves of different spatial scales are recorded, with the occurrence rate of large-scale waves increasing under undisturbed conditions. Amplitudes of the large-scale waves occurring in the magnetotail under low intensity of fluctuations outside the magnetosphere are from few tenths to a few nanoteslas (nT), and their power is approximately equal in longitudinal and transverse components. Presumably, these waves are magnetotail eigen-modes.

In this paper, we study parameters of geomagnetic pulsations in the 1–4 mHz frequency range (Pc5/Pi3) in the magnetotail, utilizing data obtained by Cluster satellites at different levels of fluctuations in the interplanetary magnetic field (IMF) and the solar wind dynamic pressure in 2016. Particular attention is given to the conditions of “zero” disturbance when amplitudes of fluctuations in the interplanetary medium are smaller compared to their typical values. Both under quiet and disturbed conditions, waves of different spatial scales are recorded, with the occurrence rate of large-scale waves increasing under undisturbed conditions. Amplitudes of the large-scale waves occurring in the magnetotail under low intensity of fluctuations outside the magnetosphere are from few tenths to a few nanoteslas (nT), and their power is approximately equal in longitudinal and transverse components. Presumably, these waves are magnetotail eigen-modes.

 magnetosphere geomagnetic pulsations magnetotail magnetosphere geomagnetic pulsations magnetotail The work was financially supported by the Russian Foundation for Basic Research, project No. 20-05-00787. The work was financially supported by the Russian Foundation for Basic Research, project No. 20-05-00787.

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