MULTIPOINT MULTIWAVELENGTH OBSERVATIONS OF A NEAR-THE-LIMB ERUPTIVE SOLAR FLARE WITH QUASI-PERIODIC PULSATIONS
Authors:
1.
Space Research Institute of the Russian Academy of Sciences
2.
Space Research Institute of Russian Academy of Sciences
Type:
Сonference article
Published:
27.12.2024
Subject area:
UDK 523.985.3 Вспышки
UDK 523.985.7 Всплески
UDK 523.987 Протуберанцы
UDK 52 Астрономия. Геодезия
UDK 53 Физика
UDK 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
UDK 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
UDK 523 Солнечная система
UDK 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
UDK 52-1 Метод изучения
UDK 52-6 Излучение и связанные с ним процессы
GRNTI 41.21 Солнце
GRNTI 41.00 АСТРОНОМИЯ
GRNTI 29.35 Радиофизика. Физические основы электроники
GRNTI 29.31 Оптика
GRNTI 29.33 Лазерная физика
GRNTI 29.27 Физика плазмы
GRNTI 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
OKSO 03.06.01 Физика и астрономия
OKSO 03.05.01 Астрономия
OKSO 03.04.03 Радиофизика
BBK 2 ЕСТЕСТВЕННЫЕ НАУКИ
BBK 223 Физика
TBK 614 Астрономия
TBK 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
UDK 523.985.7 Всплески
UDK 523.987 Протуберанцы
UDK 52 Астрономия. Геодезия
UDK 53 Физика
UDK 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
UDK 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
UDK 523 Солнечная система
UDK 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
UDK 52-1 Метод изучения
UDK 52-6 Излучение и связанные с ним процессы
GRNTI 41.21 Солнце
GRNTI 41.00 АСТРОНОМИЯ
GRNTI 29.35 Радиофизика. Физические основы электроники
GRNTI 29.31 Оптика
GRNTI 29.33 Лазерная физика
GRNTI 29.27 Физика плазмы
GRNTI 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
OKSO 03.06.01 Физика и астрономия
OKSO 03.05.01 Астрономия
OKSO 03.04.03 Радиофизика
BBK 2 ЕСТЕСТВЕННЫЕ НАУКИ
BBK 223 Физика
TBK 614 Астрономия
TBK 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
Language:
English
Keywords:
Sun: flares; X-rays, gamma rays; UV radiation; coronal mass ejections (CMEs)
Funding:
The work was supported by the Russian Science Foundation, grant 23-72-30002
Abstract (English):
We present results of the analysis of multiwavelength observations of the M3.4 eruptive flare that occurred near the western limb of the Sun on September 2, 2023 (SOL2023-09-02T06:33). We use observations from the near-Earth spacecraft ASO-S/HXI, SDO/AIA, HMI, GOES/XRS, and Fermi/GBM. X-ray observations by the STIX telescope-spectrometer on board the Solar Orbiter from the opposite side of the Sun are also used. The flare was associated with a two-stage inclined ( $\approx 40-50^{\circ}$ to the radial direction) eruption, the second stage of which was accompanied by the impulsive flare phase and quasi-periodic pulsations (QPPs) of hard X-rays with a characteristic time scale $P\approx1.56$ min. HXI observed hard X-ray sources located above the apex of a coronal Y-shaped structure, visible in the ``hot'' 94 and 131 Å EUV channels, behind a drop-shaped erupting plasmoid/prominence. Hard X-ray sources near the foot of the flare loops and flare ribbons were also observed, mainly after the peak of the impulsive phase. The HXI and STIX observations from different locations in the heliosphere are consistent with each other. Temporal dynamics of the spectral index of nonthermal electron flux had a ``soft-hard-soft'' behavior during QPPs. The observational results do not contradict the ``standard'' model of eruptive two-ribbon flares, where populations of electrons are accelerated episodically due to magnetic reconnection in a current sheet in the corona behind an erupting structure. However, understanding the quasi-periodicity of electron acceleration/injection requires further studies.
We present results of the analysis of multiwavelength observations of the M3.4 eruptive flare that occurred near the western limb of the Sun on September 2, 2023 (SOL2023-09-02T06:33). We use observations from the near-Earth spacecraft ASO-S/HXI, SDO/AIA, HMI, GOES/XRS, and Fermi/GBM. X-ray observations by the STIX telescope-spectrometer on board the Solar Orbiter from the opposite side of the Sun are also used. The flare was associated with a two-stage inclined ( $\approx 40-50^{\circ}$ to the radial direction) eruption, the second stage of which was accompanied by the impulsive flare phase and quasi-periodic pulsations (QPPs) of hard X-rays with a characteristic time scale $P\approx1.56$ min. HXI observed hard X-ray sources located above the apex of a coronal Y-shaped structure, visible in the ``hot'' 94 and 131 Å EUV channels, behind a drop-shaped erupting plasmoid/prominence. Hard X-ray sources near the foot of the flare loops and flare ribbons were also observed, mainly after the peak of the impulsive phase. The HXI and STIX observations from different locations in the heliosphere are consistent with each other. Temporal dynamics of the spectral index of nonthermal electron flux had a ``soft-hard-soft'' behavior during QPPs. The observational results do not contradict the ``standard'' model of eruptive two-ribbon flares, where populations of electrons are accelerated episodically due to magnetic reconnection in a current sheet in the corona behind an erupting structure. However, understanding the quasi-periodicity of electron acceleration/injection requires further studies.
Keywords:
Sun: flares; X-rays, gamma rays; UV radiation; coronal mass ejections (CMEs)
Sun: flares; X-rays, gamma rays; UV radiation; coronal mass ejections (CMEs)
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