[en] New index of 27-day recurrence of intensive geomagnetic perturbations during recent 100 years is suggested and calculated. Time course of this index is compared with latitudinal distribution of solar magnetic fields and protuberances during 20-th and 21-st cycles. It is shown, that solar wind flows causing essential increase and regularity in recurrence of intensive geomagnetic perturbations during drop of solar activity to the end of 11-year cycles are related with magnetic fields of activity previous 11-year cycle

[en] The results obtained from the observations of proper motions visible during the growth of local magnetic fields of active regions and during the formation and further development of their sunspot groups are summarized. It is stressed that this process is a part of the dynamics of the solar background field evolution, and the motions and shape changes observable during the whole active region's field life-time was also determined. Several types of motions and form changes during the interactions and collisions of sunspots both between themselves and with the photosphere was studied. The low efficiency of magnetic forces during the studied processes and, in contrast, the importance of hydrodynamic forces is demonstrated. The feedback action of the moving photosphere on the shape of magnetic field distribution and on the sunspot forms is presented. Problems of physical interpretation of the data presented are discussed. The importance of further observations, in the first place of the velocity fields, is underlined. (author)

[en] The degree is demonstrated to which the development of the studied flare complex is related to global changes in the solar background magnetic fields. It is connected with the action of magnetic active longitudes, it lasts about 10 rotations and, in its last phase, it forms a coronal hole. Its fields play a role in forming two sectors in the equatorial background fields and are involved in the fast global field redistribution into regular morphological patterns. All regularities found require physical interpretation. (author)

[en] In this third part of a series of papers describing the regularities in the magnetic field as well as solar activity development in a large portion of the solar atmosphere in which the processes related to the June-July 1974 proton-flare region formation take place, we study some characteristics of the solar wind which emanates from this portion of the solar atmosphere. It is shown that during the time when fast disintegration and disappearance of the large-scale characteristic magnetic field patterns occur and a sudden cease of sunspot, flare and coronal activity is observed, daily geomagnetic character figures C9 reach their maximum. This solar wind enhancement is taken as one of the last observable manifestations of the whole complex process. (author)

[en] Using more than 160 ''qualitative'' magnetic maps in series for 36 new regions, the standard features are described of the morphological development of an usual active region's magnetic field in connection with the formation of its sunspot group. A pattern was derived of magnetic field distribution for small and large active regions in their several evolutionary stages. Signs of the influence of solar differential rotation on the shape of the magnetic field, were found as well as indications of other dynamical forces acting on the active region as the photospheric matter flows around it. New facts concerning the role of the magnetic singularity in the active region's ''centre'' (centre of magnetic activity), lying in the middle part of the group at the magnetic boundary, are demonstrated. It is shown that magnetic lines of force in the ''centre'' form a subsystem, which is lower and perpendicular to the main system of magnetic lines of force joining the leading and following main spots. This subsystem seems to play a very important role in the life and in the activity of the region. (author)

[en] Previous results are summarized concerning the local magnetic field formation, showing that its sunspot groups developing to reach higher types C, D, E etc., continue their magnetic evolution during the period of new magnetic flux addition immediately after the first magnetically bipolar balanced stage. This is probably a magnetohydrodynamical process of magnetic field strengthening or a new magnetic flux generation. It is closely related to a specific singularity in the local magnetic field topology at the inner field boundary not far from the centre of the group, where the gulf of one polarity is compressed inbetween the boundary curvature of the field of opposite polarity and where large radial velocities may be observed. This is the region where new peaks of both the leading and the following polarities in a special orthogonal relation of the new to the old tubes of lines of force develop and where the greatest field gradients are formed. The flare frequencies and their importances correlate well with the degree of complexity of magnetic field topology in this situation. The important role of the photosphere in all these processes is underlined. (author). 2 figs., 30 refs

[en] Processes are investigated accompanying the formation of a very small, secondary active region during the development of its new local magnetic field on the background field through its restructuring and dissipation, as well as during the evolution of a small bipolar sunspot group. The magnetic flux values are estimated. The morphology of small sunspot transformation and two ways of their disintegration are studied. (author)

[en] Processes visible during several impulses of new sunspot formations at the periphery of an older large background magnetic field body in which one rotation earlier the large June-July 1974 proton-flare region developed are discussed. The coalescence of separate nuclei into the future umbra and the counter-clockwise rotation of the whole leading region, the change in the sense of rotation during its further development as well as the non-simultaneous development of individual parts of the active region are pointed out. (author)

[en] Using magnetic synoptic charts and daily maps preceding and following the development of the August 1972 proton-flare region in an extended time interval, it was shown that the evolution of such a complex solar process may be divided into more simple evolutionary phases. Each of the individual stages during the process of forming this complex magnetic situation may be compared with the phenomena observed during the growth of a normal complex of activity or even of a simple active region. These evolutionary stages are not only seen in the development of the magnetic field topology. They may be found in all kinds of solar activity and their occurrence in the chromosphere, corona and interplanetary space seems to depend on the successive penetration of the magnetic field lines into the higher layers of the Sun and its extensive atmosphere. (author)

[en] Results of a preliminary investigation of Mt. Wilson magnetic synoptic charts obtained during the present activity cycle are presented: in this activity cycle practically no changes in the behaviour of the magnetic field distribution are observed as compared with the preceding cycle. Also the roles of the positive and negative polarities seem to remain unaltered although their functions of leading and following polarity are exchanged. The importance of the two main recurrences or successions in the large-scale magnetic field distribution with the 27-day and 28 to 29-day synodic periods of rotation is emphasized. Shifts or ''oscillations'' of activity through the heliographic latitude are mentioned. (author)