Relativistic electron flux growth during storm and non-storm periods as observed by ARASE and GOES satellites

Belakhovsky, V.B.; Pilipenko, V.A.; Antonova, E.E.; Miyoshi, Y.; Kasahara, Y.; Kasahara, S.; Higashio, N.; Shinohara, I.; Hori, T.; Matsuda, S.; Yokota, S.; Takashima, T.; Takefumi, M.; Keika, K.; Nakamura, S.

Авторы: Belakhovsky Vladimir Borisovich, Pilipenko Vyacheslav A., Antonova Elizaveta E., Miyoshi Yoshizumi, Kasahara Yoshiya, Kasahara Satoshi, Higashio Nana, Shinohara Iku, Hori Tomoaki, Matsuda Shoya, Yokota Shoichiro, Takashima Takeshi, Takefumi Mitani, Keika Kunihiro, Nakamura Satoko
Журнал: Earth, Planets and Space
Том: 75
Номер: 1
Год издания: 2023
Издательство: Terra Scientific Publishing Company
Местоположение издательства: Japan
Номер статьи: 189
DOI: 10.1186/s40623-023-01925-1
Аннотация: Variations of relativistic electron fluxes (E ≥ 1 MeV) and wave activity in the Earth magnetosphere are studied to determine the contribution of different acceleration mechanisms of the outer radiation belt electrons: ULF mechanism, VLF mechanism, and adiabatic acceleration. The electron fluxes were measured by Arase satellite and geostationary GOES satellites. The ULF power index is used to characterize the magnetospheric wave activity in the Pc5 range. To characterize the VLF wave activity in the magnetosphere, we use data from PWE instrument of Arase satellite. We consider some of the most powerful magnetic storms during the Arase era: May 27–29, 2017; September 7–10, 2017; and August 25–28, 2018. Also, non-storm intervals with a high solar wind speed before and after these storms for comparison are analyzed. Magnitudes of relativistic electron fluxes during these magnetic storms are found to be greater than that during non-storm intervals with high solar wind streams. During magnetic storms, the flux intensity maximum shifts to lower L-shells compared to intervals without magnetic storms. For the considered events, the substorm activity, as characterized by AE index, is found to be a necessary condition for the increase of relativistic electron fluxes, whereas a high solar wind speed alone is not sufficient for the relativistic electron growth. The enhancement of relativistic electron fluxes by 1.5–2 orders of magnitude is observed 1–3 days after the growth of the ULF index and VLF emission power. The growth of VLF and ULF wave powers coincides with the growth of substorm activity and occurs approximately at the same time. Both mechanisms operate at the first phase of electron acceleration. At the second phase of electron acceleration, the mechanism associated with the injection of electrons into the region of the magnetic field weakened by the ring current and their subsequent betatron acceleration during the magnetic field restoration can work effectively.
Добавил в систему: Овчинников Илья Львович

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Relativistic electron flux growth during storm and non-storm periods as observed by ARASE and GOES satellitesстатья Исследовательская статья

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