We demonstrate that both in the global scale and in the scale of large and complex active regions the high flare activity is dosely related to the changes in the whole background magnetic field distribution. We found that the disturbances of the normal course of MALs during the years 1965 -1980 correlated with the maxima of flare activity and the mode of MALs distribution with the mean level of solar flare numbers. We showed that the development of activity during the last two ^submaxima of the 21st cycle of solar activity, especially the formation of the white-light flare region of April 1984, were parts of global processes in the solar atmosphere. They
were accompanied by a complete reorganization of the MALs patterns, background field sector structure and restructuralization of coronal holes. In both cases, in the global and in the local scales, we could follow the geophysical consequences of the entire reconstruction of global solar field amplified by the direct influence of many large flares.
In a recent paper (Olah et al., 1985) we found that the active areas of UK Lac exhibited sometimes smali, sometimes large scale motions. In the case of the Sun it is well knovvn that new spots exhibit large proper motions while the old ones move almost together with the surrounding photosphere. On UK Lac both a newly formed active area and an existing old one showed rapid motions at the same time. A possible interpretation of this phenomenon is that new spots appeared in both the new and the old active areas simultaneously. This time coincidence may be aceidental, but if spots originate in dceper layers, than spots of common decp origin may appear in remote places of the stellar surface at the same time. Similar phenomena are seen on the Sun, when we observe simultaneous emergence of new flux in various parts of an extended active region (Zirin, 1983). The distribution of the active areas on the surface of HK Lac during the past eight years, is
discussed.
Measurements of the proper niotlons of young blpolar sunspot groups show that these groups rotate faster than the surroundlng photosphere. The results of the tlme series analysis carrled out on the Irradiance records of the SMM/ACRIM radiometer and on the projected areas of the young, active sunspot groups showed a period near U days In 1980, the year of the solar maximum. The main period in the projected areas of the old sunspot groups was 28 days, which corresponded to the mean photospherlc rotatlon. The faster proper motlon of the young sunspot groups as well as the 24 days periodicity of the young active spot areas might indicate that the young sunspots are connected to the deeper regione of the Sun which rotate faster than the photosphere. Thus, the sunspot groups in the early stage of their life would be an indlcator of rotation of the deeper layers of the Sun.