THE AVERAGE SOLAR FLARE TIME PROFILES FROM OBSERVATIONS OF LOWER LAYERS OF SOLAR ATMOSPHERE DURING THE DECAY PHASE
Authors/Creators
- 1. Institute of Solar-Terrestrial Physics, SB Russian Academy of Sciences, Lermontov Str. 126a, 664033, Irkutsk, Russia
- 2. Centre for Fusion, Space and Astrophysics, Department of Physics, University of Warwick, Coventry, CV4 7AL, UK
- 3. Department of Radio Astronomical Research, Central Astronomical Observatory at Pulkovo of the RAS, Pulkovskoe Shosse 65/1, Saint Petersburg 196158, Russian Federation, Russia
- 4. Faculty of Physics, Irkutsk State University, 20 Gagarin Blvd., Irkutsk 664003, Russia
Description
We present an analysis of the decay phase of solar flares in several spectral bands using a method based on that successfully applied to white-light flares observed on an M4 dwarf. The aim of the current study was to find an averaged time profile of the solar flare decay emission coming from deep layers of the solar atmosphere and an analytical template that will best describe the evolution of emission. We selected and processed events detected in the Sun-as-a-star flux obtained with SDO/AIA images in the 1600 A and 304 and the 1700 channel. The main criterion for the selection of time profiles was a slow, continuous flux decay without significant new bursts. The obtained averaged time profiles were fitted with analytical templates, using different time intervals, that consisted of a combination of two independent exponents or a broken power law.
We discuss the possibilities of using the obtained analytical templates for describing the processes during the decay phase, the results obtained by comparing the averaged time profiles between each other. We also compared the obtained profiles with the simulated one and the stellar flare observations at the M4 dwarf.
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