INVESTIGATION OF MAGNETIC FREE ENERGY DYNAMICS IN THE M1.2-CLASS COMPLEX SOLAR FLARE OF MARCH 15, 2015 USING THE 135-SECOND HMI VECTOR MAGNETOGRAMS
Авторы:
1.
Space Research Institute of the Russian Academy of Sciences
2.
Space Research Institute of Russian Academy of Sciences
3.
Institute of Solar-Terrestrial Physics
4.
Institute of Solar-Terrestrial Physics
Тип:
Статья конференции
Опубликовано:
27.12.2024
Классификаторы:
УДК 523.985.3 Вспышки
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 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: solar flares, magnetic fields; electric currents; eruption; hard X-ray emission
Аннотация (русский):
We investigate magnetic free energy (MFE) dynamics in the M1.2 solar flare occurred on March 15, 2015, 22:45 UT. We use the nonlinear force-free field (NLFFF) model of the coronal magnetic field on the basis of 135-second HMI vector magnetograms (standard magnetograms have a temporal resolution of 720 s) from the Heliosesmic and Magnetic Imager (HMI). Since we consider a rather long event (about 100 minutes) with several episodes of energy release of different temporal dynamics (pulsed or more gradual), we can find features of the MFE dynamics relative to the flare energy release stages using 135-second vector magnetograms. It is shown that the main MFE dissipation (approximately 30 % of the initial level) occurred during the two first subflare bursts seen in microwave hard X-ray ranges. These two bursts developed at low (less than 5 Mm) magnetic structures extremely elongated along the magnetic field polarity inversion line (PIL), while the other long-lasting bursts without appreciable MFE dissipation occurred in a growing flare arcade of magnetic loops. The obtained results are in favor of the fact that most of the MFE is localized in magnetic structures with a strong electric current at the PIL. It is possible that local monitoring of the preflare state around the PIL based on magnetic extrapolations with high temporal and spatial resolution will allow further improvement of methods for predicting solar flares. The dynamics of relative helicity are also studied in relation to the dynamics of the eruptions, and we found that the first impulsive subflares were accompanied by the most significant drop in helicity.
We investigate magnetic free energy (MFE) dynamics in the M1.2 solar flare occurred on March 15, 2015, 22:45 UT. We use the nonlinear force-free field (NLFFF) model of the coronal magnetic field on the basis of 135-second HMI vector magnetograms (standard magnetograms have a temporal resolution of 720 s) from the Heliosesmic and Magnetic Imager (HMI). Since we consider a rather long event (about 100 minutes) with several episodes of energy release of different temporal dynamics (pulsed or more gradual), we can find features of the MFE dynamics relative to the flare energy release stages using 135-second vector magnetograms. It is shown that the main MFE dissipation (approximately 30 % of the initial level) occurred during the two first subflare bursts seen in microwave hard X-ray ranges. These two bursts developed at low (less than 5 Mm) magnetic structures extremely elongated along the magnetic field polarity inversion line (PIL), while the other long-lasting bursts without appreciable MFE dissipation occurred in a growing flare arcade of magnetic loops. The obtained results are in favor of the fact that most of the MFE is localized in magnetic structures with a strong electric current at the PIL. It is possible that local monitoring of the preflare state around the PIL based on magnetic extrapolations with high temporal and spatial resolution will allow further improvement of methods for predicting solar flares. The dynamics of relative helicity are also studied in relation to the dynamics of the eruptions, and we found that the first impulsive subflares were accompanied by the most significant drop in helicity.
Ключевые слова:
Sun: solar flares, magnetic fields; electric currents; eruption; hard X-ray emission
Sun: solar flares, magnetic fields; electric currents; eruption; hard X-ray emission
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