The occurrence frequency of white-light flares

Details The occurrence frequency of white-light flares The occurrence frequency of white-light flares

Oct 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...88..275n&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 88, Oct. 1983, p. 275-280.

Physics

16

Frequency Distribution, Microwaves, Solar Cycles, Solar Flares, Solar Radio Bursts, Extreme Ultraviolet Radiation, Light (Visible Radiation)

Scientific paper

An occurrence frequency for white-light flares (WLF) of 15.5 + or - 4.5/yr during a 2.6-year period following the maximum of solar cycle 21 is derived. This compares with a frequency 5-6/yr derived by McIntosh and Donnelly (1972) during solar cycle 20. It is found that the higher frequency of the more recently observed WLFs is due to the availability of patrol data at shorter wavelengths (less than about 4000 A), where the contrast of the flare emission is increased; the improved contrast has allowed less energetic (and hence more frequently occurring) events to be classified as WLFs. Sufficient conditions for the occurrence of a WLF are found to be: active region magnetic class = delta; sunspot penumbra class = K, with spot group area greater than or equal to 500 millionths of the solar hemisphere; 1-8-A X-ray burst class greater than or equal to X2.

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