Initiation and chromospheric effects of a M1.0 class solar flare from high-resolution multi-wavelength observations. Issue Volume 12:Issue S327(2016) (12th September 2017)

• Record Type: Journal Article
• Authors: Sadykov, V. M.; Kosovichev, A. G.; Sharykin, I. N.; Zimovets, I. V.; Dominguez, S. Vargas
• Editors: Vargas Domínguez, S.; Kosovichev, A.G.; Antolin, P.; Harra, L.
• Is Part Of: Proceedings of the International Astronomical Union. Volume 12:Issue S327(2016)
• Page Start: 103
• Page End: 108
• Publication Date: 2017-09-12
• Subjects: Sun: flares, -- Sun: magnetic fields, -- Sun:photosphere, -- Sun: chromosphere, -- Sun: transition region; Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S1743921317003994
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract: Initiation and development of a M 1.0 class flare of June 12, 2014, was observed by space and ground-based telescopes, including EUV and X-ray imaging spectroscopy by IRIS and RHESSI, and high-resolution optical imaging by 1.6 m New Solar Telescope (NST). Analyzing the NST data, we found small-scale loop-like structures in the region of the magnetic field Polarity Inversion Line (PIL), the emergence and interaction of which caused photospheric brightenings temporarily coinciding with hard X-ray impulses. Detailed studies of the PIL region reveal signatures of photospheric plasma downflows and dissipation of electric currents. The reconstructed magnetic field topology shows a bundle of lines connecting the PIL region with the flare ribbons which were places of chromospheric evaporation observed by IRIS. The observations suggest a scenario with the primary energy release processes located in the low atmospheric layers of the PIL, energizing the overlying large-scale magnetic structure and causing "gentle" chromospheric evaporation.