MULTIPOINT MULTIWAVELENGTH OBSERVATIONS OF A NEAR-THE-LIMB ERUPTIVE SOLAR FLARE WITH QUASI-PERIODIC PULSATIONS
Авторы:
1.
Space Research Institute of the Russian Academy of Sciences
2.
Space Research Institute of Russian Academy of Sciences
Тип:
Статья конференции
Опубликовано:
27.12.2024
Классификаторы:
УДК 523.985.3 Вспышки
УДК 523.985.7 Всплески
УДК 523.987 Протуберанцы
УДК 52 Астрономия. Геодезия
УДК 53 Физика
УДК 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
УДК 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
УДК 523 Солнечная система
УДК 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
УДК 52-1 Метод изучения
УДК 52-6 Излучение и связанные с ним процессы
ГРНТИ 41.21 Солнце
ГРНТИ 41.00 АСТРОНОМИЯ
ГРНТИ 29.35 Радиофизика. Физические основы электроники
ГРНТИ 29.31 Оптика
ГРНТИ 29.33 Лазерная физика
ГРНТИ 29.27 Физика плазмы
ГРНТИ 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
ОКСО 03.06.01 Физика и астрономия
ОКСО 03.05.01 Астрономия
ОКСО 03.04.03 Радиофизика
ББК 2 ЕСТЕСТВЕННЫЕ НАУКИ
ББК 223 Физика
ТБК 614 Астрономия
ТБК 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
УДК 523.985.7 Всплески
УДК 523.987 Протуберанцы
УДК 52 Астрономия. Геодезия
УДК 53 Физика
УДК 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
УДК 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
УДК 523 Солнечная система
УДК 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
УДК 52-1 Метод изучения
УДК 52-6 Излучение и связанные с ним процессы
ГРНТИ 41.21 Солнце
ГРНТИ 41.00 АСТРОНОМИЯ
ГРНТИ 29.35 Радиофизика. Физические основы электроники
ГРНТИ 29.31 Оптика
ГРНТИ 29.33 Лазерная физика
ГРНТИ 29.27 Физика плазмы
ГРНТИ 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
ОКСО 03.06.01 Физика и астрономия
ОКСО 03.05.01 Астрономия
ОКСО 03.04.03 Радиофизика
ББК 2 ЕСТЕСТВЕННЫЕ НАУКИ
ББК 223 Физика
ТБК 614 Астрономия
ТБК 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
Язык материала:
английский
Ключевые слова:
Sun: flares; X-rays, gamma rays; UV radiation; coronal mass ejections (CMEs)
Финансирование:
Работа выполнена при поддержке гранта РНФ № 23-72-30002
Аннотация (русский):
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.
Ключевые слова:
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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