STATISTICS OF MAGNETIC ENERGIES IN SOLAR ACTIVE REGIONS OF DIFFERENT HALE AND MCINTOSH CLASSES
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 523.982 Солнечные пятна
УДК 523.985-125 Предсказания. Прогнозирование
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 523.985-125 Предсказания. Прогнозирование
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
Язык материала:
английский
Ключевые слова:
Sun: activity, magnetic fields, sunspots, flares
Аннотация (русский):
A statistical analysis of the magnetic energies (of the nonlinear force-free and potential fields, $E_\text{NLFFF}$, $E_\text{POTF}$, and their difference - a proxy for the free magnetic energy, $E_\text{FREE}$) in active regions (ARs) on the Sun of different Hale and McIintosh classes for the period from May 1, 2010 to 12 June, 2024 ( $\approx 1.3$ solar cycles) is presented. The magnetic field in ARs is calculated using the GX Simulator based on the photospheric vector magnetograms by the Helioseismic and Magnetic Imager (HMI) anboard the Solar Dynamics Observatory (SDO) and information about ARs contained in the daily Solar Region Summary (SRS) files provided by the NOAA SWPC. Distributions of different parameters have been determined in total for all ARs and separately for each Hale and McIntosh class, the mean values of the parameters and standard deviations were calculated for each class. As expected, it is found that the magnetic energies, unsigned magnetic flux, as well as the integral number of sunspots, the number of active regions, and the area of sunspots, integrated over ARs visible per day on the solar disk, exhibit an $\approx 11$ - year cyclicity. On average, magnetic energies of ARs increase with increasing Hale and McIntosh class (with sub-peaks in $E_\text{POTF}$ and $E_\text{NLFFF}$ for Hhx, Hkx, Cho-Cki), while the average fraction of the free magnetic energy, $E_\text{FREE}/E_\text{NLFFF}$ in ARs of different classes differs weakly. Correlation between $E_\text{POTF}$ and $E_\text{NLFFF}$ is almost identical for ARs of different Hale classes with the high values of the linear Pearson correlation coefficient, $ccp$, from 0.96 to 0.99. $E_\text{FREE}$ is less correlated with $E_\text{POTF}$ and $E_\text{NLFFF}$ ($ccp$ is from 0.32 to 0.71).
A statistical analysis of the magnetic energies (of the nonlinear force-free and potential fields, $E_\text{NLFFF}$, $E_\text{POTF}$, and their difference - a proxy for the free magnetic energy, $E_\text{FREE}$) in active regions (ARs) on the Sun of different Hale and McIintosh classes for the period from May 1, 2010 to 12 June, 2024 ( $\approx 1.3$ solar cycles) is presented. The magnetic field in ARs is calculated using the GX Simulator based on the photospheric vector magnetograms by the Helioseismic and Magnetic Imager (HMI) anboard the Solar Dynamics Observatory (SDO) and information about ARs contained in the daily Solar Region Summary (SRS) files provided by the NOAA SWPC. Distributions of different parameters have been determined in total for all ARs and separately for each Hale and McIntosh class, the mean values of the parameters and standard deviations were calculated for each class. As expected, it is found that the magnetic energies, unsigned magnetic flux, as well as the integral number of sunspots, the number of active regions, and the area of sunspots, integrated over ARs visible per day on the solar disk, exhibit an $\approx 11$ - year cyclicity. On average, magnetic energies of ARs increase with increasing Hale and McIntosh class (with sub-peaks in $E_\text{POTF}$ and $E_\text{NLFFF}$ for Hhx, Hkx, Cho-Cki), while the average fraction of the free magnetic energy, $E_\text{FREE}/E_\text{NLFFF}$ in ARs of different classes differs weakly. Correlation between $E_\text{POTF}$ and $E_\text{NLFFF}$ is almost identical for ARs of different Hale classes with the high values of the linear Pearson correlation coefficient, $ccp$, from 0.96 to 0.99. $E_\text{FREE}$ is less correlated with $E_\text{POTF}$ and $E_\text{NLFFF}$ ($ccp$ is from 0.32 to 0.71).
Ключевые слова:
Sun: activity, magnetic fields, sunspots, flares
Sun: activity, magnetic fields, sunspots, flares
1. Nita G.M., Fleishman G.D., Kuznetsov A.A., et al., 2023, Astrophysical Journal Supplement Series, 267, 1, id. 6
2. Scherrer P.H., Schou J., Bush R.I., et al., 2012, Solar Physics, 275, 1-2, p. 207
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