The process of mastering the SSRT has been accompanied by an expansion of the scientific interests and a change of the requirements to its characteristics. The advent of new technologies and instrumentation made it possible to embark on the modernization of the SSRT systems. The use of SHF amplifiers with a noise temperature of 50 degrees allowed the SSRT sensitivity to be improved considerably, enabling the recording and study of low-contrast features in the solar corona: coronal holes, filament, and bright coronal points. The receiving-recording system is being improved through the use of acoustooptic facilities. The methodology of improving the solar corona radio image quality is under development. It has been possible to achieve a spatial and temporal resolution of up to 15 sec of arc and up to 14 ms, respectively.
     The relatively high angular and, especially, temporal resolution of the SSRT, together with the adequate sensitivity, made it possible to considerably extend our research to almost all forms of solar activity: new models were proposed (and the old models refined) for active regions, flares, formation and acceleration of energetic particle fluxes, coronal mass ejections, and coronal holes. First and foremost the spatial-temporal characteristics of the origination and development of active regions were studied. A detailed study was made of the phenomenon of the sign reversal of the circular polarization of emission from the active region during its solar disk passage, a number of new flare buildup signatures were identified, an effective criterion of flare ‘protonicity’ from the character of emission polarization distribution of the active region was developed, we studied the properties and