Coordinated radio observations during SMM

Combined X-UV and high resolution cm-wavelength observations conducted during SMM are discussed. The results reveal that very high magnetic fields are present at coronal levels either above very large sunspots or above small spots of the same polarity. High brightness temperature sources are sometimes observed in active regions without any association with X-ray or magnetic structures. They can be explained only by the presence of currents generating a strong nonpotential field in the corona or by a nonthermal mechanism; the high brightness temperatures seem to indicate the latter mechanism. Some results on correlated coronograph and metric wavelength observations of type II and type IV radio bursts detected during coronal transients are also presented. These indicate that the former bursts are not excited by the shock wave generated by coronal mass ejection (CME), while the latter can be generated by plasma oscillations in a denser plasmoid travelling with the CME.