Oscillations of Radiation of Solar Flares in 3 mm Range

The radio emission of the Sun in 3-mm range observations are the important source of the information about dynamics of evolution of solar active regions. The solar flares observations allow investigation the physical processes accompanying these phenomena. Their variety determines uniqueness of each solar flare. Solar flares are the result of abundant magnetic field annihilation during magnetic lines reconnection. Abundant magnetic field energy accumulation occurs at the vortex motion of the magnetized plasma of photosphere due to pressing a magnetic field and the stretching of magnetic tubes. The magnetic lines of a various direction approach results in appearance of the high-power current layers between them for compensation a tangential gap. Current layers dissipate at reconnection of magnetic lines. It causes flare high- temperature heating of plasma in the field of magnetic reconnection. Thus there are an acceleration of free electrons up to high energy and electromagnetic energy radiation by them in broad frequency band.