An Attempt to Classify Solar Microwave-Bursts by Source Localization Characteristics and Dynamics of Flare-Energy Release

Microwave fine structures allow us to study plasma evolution in an energy release region. The Siberian Solar Radio Telescope (SSRT) is a unique instrument designed to examine fine structures at 5.7 GHz. A complex analysis of data from RATAN-600, 4–8 GHz spectropolarimeter, and SSRT, simultaneously with EUV data, made it possible to localize sources of III type microwave bursts in August 10, 2011 event within the entire frequency band of burst occurrence, as well as to determine the most probable region of primary energy release. To localize sources of III type bursts from RATAN-600 data, an original method for data processing has been worked out. At 5.7 GHz, the source of bursts was determined along two coordinates, whereas at 4.5, 4.7, 4.9, 5.1, 5.3, 5.5, and 6.0 GHz, their locations were identified along one coordinate. The size of the burst source at 5.1 GHz was found to be maximum as compared to those at other frequencies.

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Sources of type III solar microwave bursts

Solnechno-Zemnaya Fizika ◽

10.12737/17341 ◽

2016 ◽

Vol 2 (2) ◽

pp. 12-21

Author(s):

Дмитрий Жданов ◽

Dmitriy Zhdanov ◽

Сергей Лесовой ◽

Sergey Lesovoi ◽

Сусанна Тохчукова ◽

...

Keyword(s):

Energy Release ◽

Complex Analysis ◽

Primary Energy ◽

Original Method ◽

Burst Source ◽

Siberian Solar Radio Telescope ◽

Solar Microwave ◽

Extreme Uv ◽

Fine Structures ◽

Microwave Bursts

Microwave fine structures allow us to study plasma evolution in an energy release region. The Siberian Solar Radio Telescope (SSRT) is a unique instrument designed to examine fine structures at 5.7 GHz. A complex analysis of data from RATAN-600, 4–8 GHz spectropolarimeter, and SSRT, simultaneously with extreme UV data, made it possible to localize sources of III type microwave drift bursts in August 10, 2011 event within the entire frequency band of burst occurrences, as well as to determine the most probable region of primary energy release. To localize sources of III type bursts from RATAN-600 data, an original method for data processing has been worked out. At 5.7 GHz, the source of bursts was determined along two coordinates whereas at 4.5, 4.7, 4.9, 5.1, 5.3, 5.5 and 6.0 GHz, their locations were identified along one coordinate. The size of the burst source at 5.1 GHz was found to be maximum as compared to source sizes at other frequencies.

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An Attempt to Classify Solar Microwave-Bursts by Source Localization Characteristics and Dynamics of Flare-Energy Release

Symposium - International Astronomical Union ◽

10.1017/s0074180900114767 ◽

1998 ◽

Vol 188 ◽

pp. 205-206

Author(s):

A. Krüger ◽

B. Kliem ◽

J. Hildebrandt ◽

V.P. Nefedev ◽

B.V. Agalakov ◽

...

Keyword(s):

Source Localization ◽

Solar Radio ◽

Spectral Characteristics ◽

Solar Radio Bursts ◽

Spatially Resolved ◽

Siberian Solar Radio Telescope ◽

Solar Microwave ◽

Magnetic Origin ◽

Flare Process ◽

Microwave Bursts

An overview of spatially resolved observations of solar radio bursts obtained by the Siberian Solar Radio Telescope at 5.8 GHz during the last ten years reveals the occurrence of different classes of burst emission defined by their source localization characteristics. Four major classes of bursts according to the source position relative to sunspots, the source size and structure, and the source height, could be tentatively distinguished and compared with burst spectral characteristics as well as with soft X-ray emission oberved by YOHKOH. These findings are in favour of a magnetic origin of the underlying flare process.

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Influence of Radio Wave Propagation on the Properties of Solar Microwave Bursts

Solar Physics ◽

10.1007/s11207-009-9410-1 ◽

2009 ◽

Vol 258 (2) ◽

pp. 267-275 ◽

Cited By ~ 5

Author(s):

Y. F. Yurovsky

Keyword(s):

Wave Propagation ◽

Radio Wave ◽

Radio Wave Propagation ◽

Solar Microwave ◽

Microwave Bursts

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Solar microwave bursts as indicators of the occurrence of solar proton emission

Solar Physics ◽

10.1007/bf00148831 ◽

1971 ◽

Vol 19 (1) ◽

pp. 152-170 ◽

Cited By ~ 26

Author(s):

David L. Croom

Keyword(s):

Solar Proton ◽

Proton Emission ◽

Solar Microwave ◽

Microwave Bursts

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Gamma-rays from Solar Flares

Symposium - International Astronomical Union ◽

10.1017/s0074180900162850 ◽

2000 ◽

Vol 195 ◽

pp. 123-132 ◽

Cited By ~ 7

Author(s):

R. Ramaty ◽

N. Mandzhavidze

Keyword(s):

Energy Release ◽

Gamma Rays ◽

Solar Flares ◽

Gamma Ray ◽

Particle Interaction ◽

Mass Motion ◽

Relativistic Electrons ◽

Total Energy Release ◽

Flare Energy ◽

Accelerated Particles

Gamma-ray emission is the most direct diagnostic of energetic ions and relativistic electrons in solar flares. Analysis of solar flare gamma-ray data has shown: (i) ion acceleration is a major consequence of flare energy release, as the total flare energy in accelerated particles appears to be equipartitioned between ≳ 1 MeV/nucleon ions and ≳ 20 keV electrons, and amounts to an important fraction of the total energy release; (ii) there are flares for which over 50% of the energy is in a particles and heavier ions; (iii) in both impulsive and gradual flares, the particles that interact at the Sun and produce gamma rays are essentially always accelerated by the same mechanism that operates in impulsive flares, probably stochastic acceleration through gyroresonant wave particle interaction; and (iv) gamma-ray spectroscopy can provide new information on solar abundances, for example the site of the FIP-bias onset and the photospheric 3He abundance. We propose a new technique for the investigation of mass motion and mixing in the solar atmosphere: the observations of gamma-ray lines from long-term radioactivity produced by flare accelerated particles.

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