On the reconstruction of the energy distribution of electrons accelerated in solar flares

Motorina, G. G.; Koudriavtsev, I. V.; Lazutkov, V. P.; Matveev, G. A.; Savchenko, M. I.; Skorodumov, D. V.; Charikov, Yu. E.

doi:10.1134/s1063784212120201

Cited by 6 publications

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“…In order to estimate F ν , the unsaturated SDO/AIA data were calibrated using the program aia_prep.pro and normalized to the exposure time for six EUV wavebands (94 Å, 131 Å, 171 Å, 193 Å, 211 Å, 335 Å). Then the differential emission measure [φ(T )] for the time interval 11:43:15 -11:43:27 UT was calculated from the area of a coronal source S c ≈ 4 × 10 18 cm 2 (Figure 7) corresponding to the 50% RHESSI contour (CLEAN algorithm, Hurford et al, 2002) in the energy range of 7 -10 keV based on the Tikhonov regularization technique (Tikhonov and Arsenin, 1979;Kontar et al, 2004Kontar et al, , 2005Hannah and Kontar, 2012;Motorina et al, 2012Motorina et al, , 2016. The results of numerical calculations of [φ(T )], averaged over the source area (Figure 8), show evidence that the coronal part of the flareenergy-release region contains a large amount of plasma with T = 0.5 -3 MK.…”

Section: Millimeter Bremsstrahlung Emission From the Coronamentioning

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Millimeter and X-Ray Emission from the 5 July 2012 Solar Flare

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The 5 July 2012 solar flare (11:39 -11:49 UT) with an increasing millimeter spectrum between 93 and 140 GHz is considered. We use space and ground-based observations in X-ray, extreme ultraviolet, microwave, and millimeter wave ranges obtained with the Reuven Ramaty High-Energy Solar Spectroscopic Imager, Solar Dynamics Observatory (SDO), Geostationary Operat ional E nvironmental Satellite, Radio Solar Telescope Network, and Bauman Moscow State Technical University millimeter radio telescope RT-7.5. The main parameters of thermal and accelerated electrons were determined through Xray spectral fitting assuming the homogeneous thermal source and thick-target model. From the data of the Atmospheric Imaging Assembly/SDO and differential emission measure calculations it is shown that the thermal coronal plasma gives a negligible contribution to the millimeter flare emission. Model calculations suggest that the observed increase of millimeter spectral flux with frequency is determined by gyrosynchrotron emission of high-energy ( $≳ 300$

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