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A set of 22 simple, impulsive solar flares, identified in the OSO-5 hard X-ray data, have been analyzed together with coincident microwave and meterwave radio observations. The rise times and fall times of the X-ray bursts are found to be highly correlated and effectively equal, strongly suggesting a flare energizing mechanism that is reversible. The good time resolution available for these observations reveals that the microwave emission is influenced by an additional process, evident in the tendency of the microwave emission to peak later and decay more slowly than the symmetric X-ray bursts. Meter-wave emission is observed in coincidence with the 5 events which show the strongest time correlation between the X-ray" and microwave burst structure. This meterwave emission is characterized by U=burst radiation, indicating confinement of the flare source. The relationship found between the X-ray burst duration and the calculated flare diameter, together with the thermal character of the X-ray spectra, gives additional support to the hypothesis that these flares are driven by adiabatic compression and expansion of a magnetically confined plasma which is the common, primary source of both X-ray and microwave emission.

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