The Balmer 9 and Balmer 11 lines of He II in the sun

Details The Balmer 9 and Balmer 11 lines of He II in the sun The Balmer 9 and Balmer 11 lines of He II in the sun

Mar 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979soph...61..271r&link_type=abstract

Solar Physics, vol. 61, Mar. 1979, p. 271-277.

Physics

11

Balmer Series, Helium, Photoionization, Solar Spectra, Gas Ionization, Recombination Reactions, Solar Flares

Scientific paper

The Balmer 9 and 11 lines of He II at 959 A and 942 A in solar spectra are identified. These lines are produced mainly by recombination following photoionization of He II by coronal XUV radiation. From analysis of the line intensities, the theoretical model of Avrett et al. (1976), is confirmed where it was found that an appreciable amount of He (2+) is present at temperatures of 1 - 2 x 10 to the 4th K and that the anomalously strong He II 304 line is produced primarily by collisional excitation. The suggestion of Kohl (1977) that the photoionization-recombination process is more important in active regions than in the quiet sun is confirmed, and we find that the 304-A line is produced largely by recombination in solar flares.

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