Using the results of solar flare observations during the SMY period (1979-1982), as well as X-ray and radio data, it was established that;
1) the flare can be considered as a complex of flare knots or brightenings, spatially and temporally distributed within the flare phenomenon. The comparison of flare knots with the flare radio source (Westerborge) and X-ray data (SMM, Hinotori) shovvs that the former provide a complete informiation about the place of the flare energy release;
2) the localization of the flare knots gives information about the flare hard X-ray and rnicrowave radiation with a flux of 300 s.f.u.;
3) by spatial order of arising flare knots the flares can be divided into three groups:
(a) the flares with a precipitant start over all ranges of electromagnetic emission are observed when the flare knots lie within sunspot groups;
(b) the flares with a gradual start are observed when the flare knots arising in the spotless area usually near a filament) penetrate into the sunspot group in the process of flare evolution;
(e) "spotless" flares are characterized by a slow rise to the maximum, a large area in Hα and very poor hard X-ray and microwave radiation;
4) the appeared flare knots are divided into two rnodules: an internal and an external one with respect to zero line of the longitudinal magnetic field. The external flare knot begins a discrete displacement, determining the appearance of new AFS. The probability of the second brightening of the same flare knot
is much smaller than of appearance of a new one.