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 41.00 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
We present the results of a study of the non-eruptive C2.8 class flare in the active region (AR) NOAA 13256, which occurred on March 19,2023 from 02:12 to 02:19 UTC. This event was chosen on the basis of the test launches of the Irkutsk Solar Radio Spectropolarimeter (SOLARSPEL), Badary (ISTP RAS). Despite the low X-ray class and short duration, according to SOLARSPEL data, this impulsive flare had a complex multi-peak fine time structure, recorded at different frequencies in the microwave range. The presence of a photospheric disturbance in the vicinity of the sunspot penumbra, recorded using HMI/SDO, was of great interest for physics and motivated this study. There are few detailed multi-wavelength studies in the literature of low-power flares accompanied by a response at the photosphere level. Notably, this event was observed simultaneously by four X-ray instruments: SoLO/STIX, ASO-S/HXI, FERMI/GBM, and Konus-Wind. As a result, the unique observation conditions of this flare, from the point of view of the available instruments and various recorded physical high-energy processes, motivated us to carry out detailed research. We found that the photospheric perturbations are mostly associated with the stronger magnetic field in the penumbra rather than with the distribution of the HXR sources. The observed flare ribbons were located in the penumbral PIL region, which revealed the complexity of the larger events in terms of the spatial and temporal structure of the energy release. We also briefly discuss the observed quasi-periodic pulsations.
Sun: solar flare, radio emission, X-ray emission, photospheric perturbations, magnetic fields
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