Helium resonance lines in the flare of 15 June 1973

Details Helium resonance lines in the flare of 15 June 1973 Helium resonance lines in the flare of 15 June 1973

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989soph..120..309p&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 120, no. 2, 1989, p. 309-341.

Physics

4

Helium, Photoionization, Resonance Lines, Solar Flares, Solar Spectra, Atmospheric Models, Helium Atoms, Solar Corona, Spectroheliographs

Scientific paper

Time sequences of He I and He II resonance line intensities at several sites within the flare of June 15, 1973 are derived from observations obtained with Naval Research Laboratory's Slitless Spectroheliograph on Skylab. The data are compared with predictions in six model flare atmospheres based on two values for the heating rate and three for the flux of photoionizing coronal X-rays and EUV. A peak ionizing flux more than 1000 times that in the quiet sun is indicated. Implications for the common practice of deriving stellar coronal fluxes from He II 1640 A fluxes assuming dominance of the recombination mechanism, are discussed.

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