Development of solar energetic particle sources within the background magnetic fields

Abstract

The greatest coronal and interplanetary disturbances are considered consequences of complex processes accompanying development of large-flare regions. Such regions not only possess a specific magnetic field configuration, but their magnetic topology develops following certain rules within the frame of slowly changing large-scale distribution of the background magnetic field patterns as a result of the mutual influences of new magnetic flux appearance as well as old field weakening and dissipation. In this paper we try to demonstrate the individual phases of the large-scale long lasting magnetic field pattern formation with their morphological characteristics and magnetic field configurations. The time scale of the whole process is shown, and the possible reasons of such development are discussed. The proton flare regions of August 1972 and July 1974 are used as examples of the successive magnetic field complication and strengthening, the result of which is the appearance of still more complicated magnetic and velocity fields that produces proton flares and then the fast disintegration of the whole magnetic situation occupying more than one half of the visible solar surface following the occurrence of the proton flares. The consequences which may be used for the proton flare prediction are discussed.