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Resolving the Spatial Configuration of X-ray Spikes in Magnetoactive Plasma: The July 3, 2017 Solar Flare
Russian version
Charikov Yu. E. 1, Shuvalova V. I. 2, Sklyarova E. M. 1, Shabalin A. N. 1,3
1Ioffe Institute, St. Petersburg, Russia
2Pulkovo Astronomical Observatory, Russian Academy of Sciences, St. Petersburg, Russia
3Institute of Space Research, Russian Academy of Sciences, Moscow, Russia
Email: Yuri.Charikov@mail.ioffe.ru, sklyarova.mhd@mail.ioffe.ru
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In this study, the spatial distribution of the sources of subsecond bursts (spikes) of hard X-ray radiation was analyzed according to data detected during solar flares by the Konus-Wind, CGRO/BATSE, YOHKOH/HXT, RHESSI, and Fermi GBM spectrometers. An analysis of the temporal structure of hard X-ray emissions from 10 behind-the-limb events revealed spikes in two of them. The SOL2017-07-03T16 : 13 : 22 flare (class M1.3) showed spikes in the energy range of 11 to 100 keV during the flux growth stage. The Fermi GBM spectrometer recorded individual spikes with durations of approximately 300-700 ms. The analysis of spatial images of the sources in the EUV lines 171, 94, and 131 Angstrem during this event determined their locations in the upper part of the loop structure of the flare's magnetic field. Keywords: solar flares, X-rays, EUV, spikes, acceleration.
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