Sources of type III solar 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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Sources of type III solar microwave bursts

Solar-Terrestrial Physics ◽

10.12737/20996 ◽

2016 ◽

Vol 2 (2) ◽

pp. 15-27 ◽

Cited By ~ 1

Author(s):

Дмитрий Жданов ◽

Dmitriy Zhdanov ◽

Сергей Лесовой ◽

Sergey Lesovoi ◽

Сусанна Тохчукова ◽

...

Keyword(s):

Energy Release ◽

Complex Analysis ◽

Primary Energy ◽

Original Method ◽

Burst Source ◽

Energy Release Region ◽

Siberian Solar Radio Telescope ◽

Solar Microwave ◽

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

The Hot Universe ◽

10.1007/978-94-011-4970-9_47 ◽

1998 ◽

pp. 205-206

Author(s):

A. KrüGer ◽

B. Kliem ◽

J. Hildebrandt ◽

V. P. Nefedev ◽

B. V. Agalakov ◽

...

Keyword(s):

Energy Release ◽

Source Localization ◽

Flare Energy ◽

Solar Microwave ◽

Microwave Bursts

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Evidence for Reality of Rapid Solar Radio Fluctuation

International Astronomical Union Colloquium ◽

10.1017/s0252921100029377 ◽

1993 ◽

Vol 141 ◽

pp. 355-358

Author(s):

Fu Qijun ◽

Hu Chumin ◽

Zhao Bing ◽

Jin Shenzhen ◽

Yu. Yurovsky ◽

...

Keyword(s):

Conclusive Evidence ◽

High Time Resolution ◽

Frequency Range ◽

Applied Physics ◽

Solar Microwave ◽

Fine Structures ◽

University Of Bern ◽

Puzzling Problem ◽

First Time ◽

Microwave Bursts

Since fast fine structures (FFS) superimposed on microwave bursts were found with high time resolution observations, they have been observed in extensive frequency range (Slottje 1978; Fu, et al. 1986; Stähli and Magun 1986; and Stepanov and Yurovsky 1991), and these results make understanding of the emission deepening. But, at the same time, the puzzling problem, these phenomena originate from sun or are only artificial, is often concerned and disputed (Benz and Fürst 1987). As it was pointed out by Benz and Fürst (1987), “the only really reliable way to study solar microwave fluctuation is to use two or more widely separated radio telescopes”.In this paper, some of FFS events superimposed on microwave bursts simultaneously obtained at Beijing Astronomical Observatory (BAO), Crimea Astrophysical Observatory (CAO) and Institute of Applied Physics, University of Bern (IAP), are presented at first time. It is a conclusive evidence of rapid radio fluctuation originating from sun and associated with flare appearance.

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A New Catalogue of Fine Structures Superimposed on Solar Microwave Bursts

Chinese Journal of Astronomy and Astrophysics ◽

10.1088/1009-9271/4/2/176 ◽

2004 ◽

Vol 4 (2) ◽

pp. 176-188 ◽

Cited By ~ 15

Author(s):

Qi-Jun Fu ◽

Yi-Hua Yan ◽

Yu-Ying Liu ◽

Min Wang ◽

Shu-Juan Wang

Keyword(s):

Solar Microwave ◽

Fine Structures ◽

Microwave Bursts

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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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