Analysis of a white-light flare spectrum

Details Analysis of a white-light flare spectrum Analysis of a white-light flare spectrum

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...98..255b&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 98, Aug. 1985, p. 255-266.

Physics

19

Solar Flares, Solar Spectra, Visible Spectrum, Continuous Spectra, Emission Spectra, H Alpha Line, Paschen Series, Spectrum Analysis

Scientific paper

The continuum emission of an X1 flare on 26 March, 1970 observed close to the solar limb (N05 E64) was analyzed by a photometric determination of the contrast ΔI(λ)/I0(λ) in the wavelength range 3558 - 5920 Å. Two possible mechanisms for the emission were investigated, namely hydrogen Paschen and H- continua. The authors show the unlikeness of the Paschen possibility and derive strong constraints on the temperature structure and energy deposition mechanism imposed by the H- continuum process. They conclude that the emission must have originated in deep atmospheric layers. The relevance of this result with respect to flare energy release and transport processes is also discussed.

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