The Basic Units of Fast Fine Structures of Solar Microwave Bursts

After the international joint observation of the Flares 22 program and Max 91 Campaign, our high time-resolution data observed with fast-sampling radiotelescopes at three frequencies(1.42, 2.28, and 3.67GHz) and four frequencies (1.42, 2.00, 2.84, and 4.00 GHz) or (1,42, 2.13, 2.84, and 4.26 GHz) were processed. Besides finding the fourth basic component of the solar radio emission, which generates on a partial region of the rati io burst source, three basic time units on the fast fine structures of solar microwave bursts are discovered. Their order of magnitude of time are 0.1s >τ₁ >lms; ls >τ₂ >0.1s; 100s >τ₃ >ls respectively. Even though the morphological properties of fast fine structures occurred on every basic time unit are different, the characteristice superimposed on the radio burst is their common property. The confirmation of three basic time units provides the scientific basic for study the fine time structures of solar microwave fast activities and for separation of the category of fast fine structures. The study of three basic time unite has a scientific significance for research on the theory of electron cyclotron maser generated in the source of fast fine structures of solar microwave bursts.