It is intended to use the mode of sequential obtaining of images at different frequencies in order to study coronal magnetic fields, in addressing problems of predicting solar activity, and in investigating low-contrast structures such as coronal holes and filaments. Coronal mass ejections are commonly characterized by the angular size as large as several tens of min of arc. Therefore, it is more appropriate to investigate such phenomena in the mode of sequential obtaining full solar images at different frequencies. Observations of ejections in the mode of simultaneous obtaining a full solar image are appropriate only when accompanied by fast occurring processes. For investigating the dynamics of solar activity (flares and, possibly, coronal mass ejections), it is intended to use the mode of simultaneous obtaining of a full solar image at 5.7 GHz  frequency and high spatial harmonics of corresponding images at the other wavelengths. A tentative configuration of antennas for this mode is illustrated in Fig. 6. The field of view for frequencies above 5.7 GHz in this case will be reduced to a few min of arc. This should not have a substantial influence on the observations of flares as a consequence of their small angular size. However, in observations of coronal mass ejections, such a limitation could have a serious influence.      It should be noted that the question as to the selection of the antenna configuration for simultaneous obtaining of images at different frequencies is open. It seems most likely that it will be answered in the process of observations. For this it is important that the whole instrument has a sufficient flexibility. Such a flexibility is ensured by equipping each antenna with a controlled multiwave receiver and by the control of the process of calculating cross-correlation functions of signals received from antennas.