  We study flare processes in the lower solar atmosphere using observational
data for a 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
understand triggers and manifestations of the flare energy release in the lower
layers of the solar atmosphere (the photosphere and chromosphere) using
high-resolution optical observations and magnetic field measurements. We
analyze optical images, HMI Dopplergrams and vector magnetograms, and use
Non-Linear Force-Free Field (NLFFF) extrapolations for reconstruction of the
magnetic topology. The NLFFF modelling reveals interaction of oppositely
directed magnetic flux-tubes in the PIL. These two interacting magnetic flux
tubes are observed as a compact sheared arcade along the PIL in the
high-resolution broad-band continuum images from NST. In the vicinity of the
PIL, the NST H alpha observations reveal formation of a thin three-ribbon
structure corresponding to the small-scale photospheric magnetic arcade.
Presented observational results evidence in favor of location of the primary
energy release site in the dense chromosphere where plasma is partially ionized
in the region of strong electric currents concentrated near the polarity
inversion line. Magnetic reconnection may be triggered by two interacting
magnetic flux tubes with forming current sheet elongated along the PIL.
