Millimeter and X-Ray Emission from the 5 July 2012 Solar Flare |
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| Authors: | Y T Tsap V V Smirnova G G Motorina A S Morgachev S A Kuznetsov V G Nagnibeda V S Ryzhov |
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| Institution: | 1.Crimean Astrophysical Observatory,Nauchny,Russia;2.Pulkovo Observatory,St. Petersburg,Russia;3.Sobolev Astronomical Institute,Saint Petersburg State University,St. Petersburg,Russia;4.University of Turku,Turku,Finland;5.Radiophysical Research Institute of Lobachevsky University,Nizhny Novgorod,Russia;6.Bauman Moscow State Technical University,Moscow,Russia |
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| Abstract: | The 5 July 2012 solar flare SOL2012-07-05T11:44 (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 Operational Environmental 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 X-ray 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 (\(\gtrsim 300\) keV) electrons in the chromosphere. The consequences of the results are discussed in the light of the flare-energy-release mechanisms. |
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