ИСТИНА

We present study of influence 3-min sunspot oscillations in initiation and evolution of the C1.5 flare June 7, 2012. The complex study of the flare was carried out based on the chromospheric observations of the solar spectrograph in Ondrejov, HXR data by RHESSI and FERMI, the microwaves data obtained with the Nobeyama Radioheliograph (NoRH, 17 GHz) and EUV observations by the Solar Dynamic Observatory (SDO/AIA, 171A). Previous study of the hard X-ray data found that emission in the 3-12 keV X-ray flux demonstrated the flat period with duration about 10 minutes while the duration of all the flare was almost 20 minutes. The "flat emission" period was also observed in 5-17 GHz. Analysis of the H-alpha slit-jaw images revealed the motion of the flare source from the spot to south direction during this period. The quasi-periodic pulsations were detected in evolution of the electron temperature. Evolution of the flare plasma parameters obtained from HXR observations indicate to presence of the explosive chromospheric evaporation followed by the impulsive phase. The oscillations in microwave and ultraviolet emission during the flare were analyzed with with pixelised wavelet filtering method (PWF) applied to high-resolution images. The appearance of the burst loop structure during maximum energy release in radio showed that one of the loop footpoint is anchored in nearest sunspot. In the ultraviolet, part of the loop coincides with the magnetic fan, where propagation of 3-min waves was found. Observed originating of fine elements as elongated structures (wakes of 3-min oscillations), directed to maximum brightness of the flare. Their appeared after impulsive phase with duration about 10 min and coincided in space with the magnetic fan. These structures can be interpreted as a waveguide for 3-min waves from sunspot. We suppose that wave energy, coming from sunspot to flare can be kept up the energy release by suppressing of plasma thermal conductivity.