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We study flare processes in the solar atmosphere using observational data fora M1-class flare of June 12, 2014, obtained by New Solar Telescope (NST/BBSO)and Helioseismic Magnetic Imager (HMI/SDO). The main goal is to understandtriggers and manifestations of the flare energy release in the photosphere andchromosphere using high-resolution optical observations and magnetic fieldmeasurements. We analyze optical images, HMI Dopplergrams and vectormagnetograms, and use Non-Linear Force-Free Field (NLFFF) extrapolations forreconstruction of the magnetic topology and electric currents. The NLFFFmodelling reveals interaction of two magnetic flux ropes with oppositelydirected magnetic field in the PIL. These flux ropes are observed as a compactsheared arcade along the PIL in the high-resolution broad-band continuum imagesfrom NST. In the vicinity of PIL, the NST H alpha observations reveal formationof a thin three-ribbon structure corresponding to a small-scale photosphericmagnetic arcade. The observational results evidence in favor of location of theprimary energy release site in the chromospheric plasma with strong electriccurrents concentrated near the polarity inversion line. In this case, magneticreconnection is triggered by the interacting magnetic flux ropes forming acurrent sheet elongated along the PIL.

Flare Energy Release in the Lower Solar Atmosphere Near the Magnetic Field Polarity Inversion Line