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Dynamics of hot chromospheric plasma of solar flares is a key tounderstanding of mechanisms of flare energy release and particle acceleration.A moderate M1.0 class flare of 12 June, 2014 (SOL2014-06-12T21:12) wassimultaneously observed by NASA's Interface Region Imaging Spectrograph (IRIS),other spacecraft, and also by New Solar Telescope (NST) at the BBSO. This paperpresents the first part of our investigation focused on analysis of the IRISdata. Our analysis of the IRIS data in different spectral lines reveals strongredshifted jet-like flow with the speed of ~100 km/s of the chromosphericmaterial before the flare. Strong nonthermal emission of the C II k 1334.5 Aline, formed in the chromosphere-corona transition region, is observed at thebeginning of the impulsive phase in several small (with a size of ~1 arcsec)points. It is also found that the C II k line is redshifted across the flaringregion before, during and after the impulsive phase. A peak of integratedemission of the hot (1.1 MK) plasma in the Fe XXI 1354.1 A line is detectedapproximately 5 minutes after the integrated emission peak of the lowertemperature C II k. A strong blueshift of the Fe XXI line across the flaringregion corresponds to evaporation flows of the hot chromospheric plasma with aspeed of 50 km/s. Additional analysis of the Reuven Ramaty High-Energy SolarSpectroscopic Imager (RHESSI) data supports the idea that the upperchromospheric dynamics observed by IRIS has features of "gentle" evaporationdriven by heating of the solar chromosphere by accelerated electrons and by aheat flux from the flare energy release site.

Properties of chromospheric evaporation and plasma dynamics of a solar flare from IRIS observations