RADIO SPECTROSCOPY OF THE SOLAR CORONA
Authors:
1.
St. Petersburg Branch of the Special Astrophysical Observatory of the Russian Academy of Sciences
St. Petersburg, Russian Federation
St. Petersburg, Russian Federation
2.
St. Petersburg Branch of the Special Astrophysical Observatory of the Russian Academy of Sciences
3.
St. Petersburg Branch of the Special Astrophysical Observatory of the Russian Academy of Sciences
4.
St. Petersburg Branch of the Special Astrophysical Observatory of the Russian Academy of Sciences
5.
St. Petersburg Branch of the Special Astrophysical Observatory of the Russian Academy of Sciences
Type:
Сonference article
Published:
27.12.2024
Subject area:
UDK 523.9 Солнце. Физика Солнца
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 41.00 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 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 41.00 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: corona, radio radiation
Funding:
Observations with the SAO RAS telescopes are supported by the Ministry of Science and Higher Education of the Russian Federation. The renovation of telescope equipment is currently provided within the national project ``Science and Universities''.
Abstract (English):
The presence of continuous cooling and heating processes is a crucial condition that determines the existence of the solar corona. The defining aspects of the corona include the magnetic field, low plasma density, and high temperature of the corona. In this regard, the study of low-contrast structures in optical ranges is limited even with the use of large specialized telescopes. The radio range provides higher sensitivity, which can be used to detect very weak structures of emerging activity. However, the radio astronomical range also faces challenges in observation, both in terms of spatial resolution and the limitations of dynamic range due to the high temperature of the Sun's corona. Observations show that the use of instruments with a large effective area allows us to overcome the main problem associated with the influence of powerful radiation from the quiet Sun, which amplifies equipment noise. The high sensitivity of the RATAN-600 reflector radio telescope to weak signals in radiation flux was used in the decimeter range for the detection of weak microwave bursts at a level of $10^{-3}$ s.f.u. Research and theoretical developments have shown that microwave bursts are caused by magnetic reconnection, which leads to the generation of accelerated particles that excite plasma waves at the second harmonic of the plasma frequency. Due to significant changes in the concept of radio spectroscopy, work has begun on creating a series of broadband spectral complexes covering several octaves. The results of the first series of observations using the complex in the range of 1-3 GHz for searching for and studying quasi-periodic pulsations in the solar corona are presented here. A by-product of these observations was the detection of narrow-band absorption in the frequency range 1560-1665 MHz, near the well-known OH absorption line (1612-1720 MHz).
The presence of continuous cooling and heating processes is a crucial condition that determines the existence of the solar corona. The defining aspects of the corona include the magnetic field, low plasma density, and high temperature of the corona. In this regard, the study of low-contrast structures in optical ranges is limited even with the use of large specialized telescopes. The radio range provides higher sensitivity, which can be used to detect very weak structures of emerging activity. However, the radio astronomical range also faces challenges in observation, both in terms of spatial resolution and the limitations of dynamic range due to the high temperature of the Sun's corona. Observations show that the use of instruments with a large effective area allows us to overcome the main problem associated with the influence of powerful radiation from the quiet Sun, which amplifies equipment noise. The high sensitivity of the RATAN-600 reflector radio telescope to weak signals in radiation flux was used in the decimeter range for the detection of weak microwave bursts at a level of $10^{-3}$ s.f.u. Research and theoretical developments have shown that microwave bursts are caused by magnetic reconnection, which leads to the generation of accelerated particles that excite plasma waves at the second harmonic of the plasma frequency. Due to significant changes in the concept of radio spectroscopy, work has begun on creating a series of broadband spectral complexes covering several octaves. The results of the first series of observations using the complex in the range of 1-3 GHz for searching for and studying quasi-periodic pulsations in the solar corona are presented here. A by-product of these observations was the detection of narrow-band absorption in the frequency range 1560-1665 MHz, near the well-known OH absorption line (1612-1720 MHz).
Keywords:
Sun: corona, radio radiation
Sun: corona, radio radiation
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