Solar-Terrestrial Physics Solar-Terrestrial Physics Solar-Terrestrial Physics 2500-0535 57605 10.12737/stp-93202307 Results of current research Results of current research Results of current research Influence of geomagnetic disturbances on scintillations of GLONASS and GPS signals as observed on the Kola Peninsula Influence of geomagnetic disturbances on scintillations of GLONASS and GPS signals as observed on the Kola Peninsula Белаховский Владимир Борисович Belahovskiy Vladimir Borisovich belakhov@mail.ru

кандидат физико-математических наук;

candidate of physical and mathematical sciences;

 Будников Павел Алексеевич Budnikov Pavel Alekseevich pavel9860@gmail.com https://orcid.org/0000-0001-7299-6546 Калишин Алексей Сергеевич Kalishin Alexey Sergeevich askalishin@aari.ru

кандидат технических наук;

candidate of technical sciences;

 Пильгаев Сергей Васильевич Pilgaev Sergey Vasilyevich pilgaev@pgia.ru Ролдугин Алексей Валентинович Roldugin Alexey Valentinovich Полярный геофизический институт Апатиты Россия Polar Geophysical Institute Apatity Russian Federation Институт прикладной геофизики им акад. Е.К. Федорова Москва Россия Institute of Applied Geophysics them. E.K. Fedorov Moscow Russian Federation Арктический и антарктический научно-исследовательский институт Санкт-Петербург Россия Arctic and Antarctic Research Institute St. Petersburg Russian Federation Полярный геофизический институт Апатиты Россия Polar Geophysical Institute Apatity Russian Federation Полярный геофизический институт Апатиты Россия Полярный геофизический институт Апатиты Russian Federation 30 09 2023 30 09 2023 9 3 54 67 09 03 2023 02 05 2023 https://naukaru.ru/en/nauka/article/57605/view

We have compared effects of geomagnetic disturbances during magnetic storms of various types (CME and CIR) and during an isolated substorm on scintillations of GLONASS and GPS signals, using a Septentrio PolaRx5 receiver installed in Apatity (Murmansk Region, Russia). We analyze observational data for 2021. The magnetic storms of November 3–4, 2021 and October 11–12, 2021 are examined in detail. The November 3–4, 2021 magnetic storm was one of the most powerful in recent years. The analysis shows that the scintillation phase index reaches its highest values during nighttime and evening substorms (σϕ≈1.5–1.8), accompanied by a negative bay in the magnetic field. During magnetic storms, positive bays in the magnetic field, associated with an increase in the eastward electrojet, lead, however, to quite comparable values of the phase scintillation index. An increase in phase scintillations during nighttime and evening disturbances correlates with an increase in the intensity of ULF waves (Pi3/Pc5 pulsations) and with the appearance of aurora arcs. This confirms the important role of ULF waves in forming the auroral arc and in developing ionospheric irregularities. The predominance of the green line in the spectrum of auroras indicates the contribution of disturbances in the ionospheric E layer to the scintillation increase. Pulsating auroras, associated with ionospheric disturbances in the D layer, do not lead to a noticeable increase in phase scintillations. Analysis of ionospheric critical frequencies according to ionosonde data from the Lovozero Hydrometeorological Station indicates the contribution of the sporadic Es layer of the ionosphere to jumps in phase scintillations. The difference between phase scintillation values on GLONASS and GPS satellites during individual disturbances can be as great as 1.5 times, which may be due to different orbits of the satellites. At the same time, the level of GLONASS/GPS scintillations at the L2 frequency is higher than at the L1 frequency. We did not find an increase in the amplitude index of scintillations during the events considered.

We have compared effects of geomagnetic disturbances during magnetic storms of various types (CME and CIR) and during an isolated substorm on scintillations of GLONASS and GPS signals, using a Septentrio PolaRx5 receiver installed in Apatity (Murmansk Region, Russia). We analyze observational data for 2021. The magnetic storms of November 3–4, 2021 and October 11–12, 2021 are examined in detail. The November 3–4, 2021 magnetic storm was one of the most powerful in recent years. The analysis shows that the scintillation phase index reaches its highest values during nighttime and evening substorms (σϕ≈1.5–1.8), accompanied by a negative bay in the magnetic field. During magnetic storms, positive bays in the magnetic field, associated with an increase in the eastward electrojet, lead, however, to quite comparable values of the phase scintillation index. An increase in phase scintillations during nighttime and evening disturbances correlates with an increase in the intensity of ULF waves (Pi3/Pc5 pulsations) and with the appearance of aurora arcs. This confirms the important role of ULF waves in forming the auroral arc and in developing ionospheric irregularities. The predominance of the green line in the spectrum of auroras indicates the contribution of disturbances in the ionospheric E layer to the scintillation increase. Pulsating auroras, associated with ionospheric disturbances in the D layer, do not lead to a noticeable increase in phase scintillations. Analysis of ionospheric critical frequencies according to ionosonde data from the Lovozero Hydrometeorological Station indicates the contribution of the sporadic Es layer of the ionosphere to jumps in phase scintillations. The difference between phase scintillation values on GLONASS and GPS satellites during individual disturbances can be as great as 1.5 times, which may be due to different orbits of the satellites. At the same time, the level of GLONASS/GPS scintillations at the L2 frequency is higher than at the L1 frequency. We did not find an increase in the amplitude index of scintillations during the events considered.

 ionosphere GLONASS GPS magnetic storm substorm aurora ionosphere GLONASS GPS magnetic storm substorm aurora The work was financially supported by the Russian Science Foundation (Grant No. 18-77-10018 (Belakhovsky V.B.)) The work was financially supported by the Russian Science Foundation (Grant No. 18-77-10018 (Belakhovsky V.B.))

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