The SSRT is a crossed interferometer operating at 5.2 cm wavelength and comprising 256 antennas 2.5 m in diameter each, arranged in the form of 128 antennas at 4.9 m intervals along the north-south and east-west directions (Fig. 1). The SSRT’s field of view is on the order of 90 min of arc. Some redundancy of the number of antenna elements was admitted in order to achieve higher sensitivity, good quality of the spectrum of spatial frequencies, and to simplify the phasing problem and the baseline for a further development of the instrument. Sequential-continuous recording of the radio brightness distribution of the solar corona is carried out through parallel multichannel reception of emission during the Sun’s transit through diffraction maxima (occupying the sky) using the frequency-dependence of the beam orientation (“scanning” in declination in the frequency band 112 MHz,  Fig. 2) and rotation of Earth (scanning in the hour angle). The frequency band that is required for collecting signals from the antennas via the branched parallel- cascaded waveguide system, was 120 MHz.  The initial signal frequency is converted twice. Parallel recording is carried out via 180 channels of 500 kHz width. All this provides solar radio images every several minutes (see examples in Figs. 3 and 4). Simultaneous records are taken of the responses of one-dimensional arrays of the instrument which are used to study fast processes during flares with a time resolution of 14 ms. Main SSRT parameters are presented in Table 1.