Phenomenology of the subflare - A synthesis of CINOF

Details Phenomenology of the subflare - A synthesis of CINOF Phenomenology of the subflare - A synthesis of CINOF

Jan 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975soph...40..133d&link_type=abstract

Solar Physics, vol. 40, Jan. 1975, p. 133-140.

Physics

5

Chromosphere, H Alpha Line, Solar Flares, Solar Magnetic Field, Solar X-Rays, Brightness, Luminous Intensity, Particle Flux Density, Phenomenology, Solar Physics, Solar Radio Emission

Scientific paper

The principal results of a coordinated investigation, conducted by many observatories, of small chromospheric brightenings, subflares, and Class 1 flares are summarized. Ten events were selected for detailed study. It was found that flares and subflares tend to occur close to, and often at either side of the neutral line. There is no clear relation between the complexity of the field and the H-alpha brightness, but there is correlation with the intensity, impulsivity, and hardness of X-ray emission and the intensity of radio emission. Filament activity may precede flare occurrences, indicating the origin of a disturbance of the active region before the flare. One case is reported where a flare occurred when erupted material had fallen down, but not at the apparent place of impact. In general, the infall of erupted material does not seem to be an important source of flare production.

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