Analysis of the August 7, 1972 white light flare - Its spectrum and vertical structure

Details Analysis of the August 7, 1972 white light flare - Its spectrum and vertical structure Analysis of the August 7, 1972 white light flare - Its spectrum and vertical structure

Oct 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974soph...38..499m&link_type=abstract

Solar Physics, vol. 38, Oct. 1974, p. 499-516.

Physics

31

Emission Spectra, Light (Visible Radiation), Line Spectra, Solar Flares, Solar Spectra, Astronomical Models, Balmer Series, Continuous Spectra, Depth Measurement, Filtergrams, Free Radicals, H Alpha Line, Iron, Molecular Spectra, Solar Activity Effects

Scientific paper

Spectral data on a white light wave occurring during the explosive phase of the August 7 flare were obtained simultaneously with three telescopes at the Sacramento Peak Observatory. Spectrograms in the wavelength region from 3530 to 5895 A and sequences of filtergrams at 4950 and 5900 A constitute the most complete record of white light flare emission obtained to date. Analysis of the iron line spectrum and of the CN and CH molecular lines shows that the maximum depth of the emission in the flare wave is about 200 km above the photosphere of the Harvard-Smithsonian Reference Atmosphere. From the Balmer line analysis, it is concluded that, in agreement with Canfield (1974) and Shmeleva and Syrovatskii (1973), the flare occurs in a thin layer and that the heating and ionization of the flaring layers are due to the injection of 100 keV electrons. There is no need to postulate filamentary structure in the flaring layer in order to explain the observations.

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