2. Solar flares. Radio methods are no less sensitive to observations of high-energy electrons than X-ray methods. Through the use of several frequencies it will be possible to determine the spectral index of emitting electrons, and the picture of the polarization - the direction of magnetic fields. In many cases it is possible to observe weaker structural elements and understand the topology of flare loops. Determination of the magnitudes of magnetic fields in the flaring region - the most important parameter for estimating the energy release. Observation of the shortest-duration manifestations of solar activity associated with plasma mechanisms of generations. In the study of flares it is also planned to use one-dimensional observations with high temp[oral resolution.
     3. Coronal mass ejections. As demonstrated by experience of investigating the CME that occurred on September 4, 2000, radio mapping provides essentially new information about the origin of coronal mass ejections. The MWRH spectral range make sit possible to investigate the process of CME development from the lower corona to altitudes on the order of one solar radius (at the background of the solar disk and in the height range inaccessible to observations in the H-alpha line, SOHO coronographs, and to m-radioheliographs). Simultaneous observations of all Sun in microwave emission will make it possible to study the association of CMEs with other forms of solar activity: flares, shock waves, and filament eruption.