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27. The dependence of flare energetics on the localization and evolution of flare knots

Creator:
Ishkov, V. N.
Format:
bez média and svazek
Type:
model:article and TEXT
Subject:
solar observations and flare knots
Language:
Czech
Description:
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.
Rights:
http://creativecommons.org/publicdomain/mark/1.0/ and policy:public