Determination of certain parameters and the fine structure of chromospheric flares

Details Determination of certain parameters and the fine structure of chromospheric flares Determination of certain parameters and the fine structure of chromospheric flares

Feb 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977azh....54..123b&link_type=abstract

Astronomicheskii Zhurnal, vol. 54, no. 1, 1977, p. 123-129. In Russian.

Astronomy and Astrophysics

Astronomy

Chromosphere, Electron Energy, Fine Structure, H Alpha Line, Optical Thickness, Solar Flares, Doppler Effect, Solar Prominences, Solar Spectra, Solar Temperature, Temperature Effects

Scientific paper

A spectral-line method is outlined for the codetermination of the H-alpha line-center optical depth, electron temperature, and emission measure of chromospheric flares. By analyzing spectrograms of one such flare, a lower limit of 7500 K is determined for the flare kinetic temperature. With respect to fine structure, it is suggested that after the maximum phase, the flare filaments expand and then combine into a much larger filament of lesser density; afterwards, the filamentary structure gradually disappears.

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