Solar coronal observations and formation of the He II 304 A line

Details Solar coronal observations and formation of the He II 304 A line Solar coronal observations and formation of the He II 304 A line

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...406..346j&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 406, no. 1, p. 346-349.

Other

23

Emission Spectra, Helium, Resonance Lines, Solar Corona, Solar Flares, Nonequilibrium Thermodynamics, Photoionization

Scientific paper

Although a large body of recent work supports the formation of the He II 304 A resonance line by collisional excitation in the quiet sun, the formation mechanism is less clear in strong coronal active regions and flares. The 1989 May 5 flight of the Goddard Solar Extreme Ultraviolet Rocket Telescope and Spectrograph (SERTS-3) provided a data set that is well suited to addressing this question. This paper develops a method of assessment of the line formation mechanism that is based on simple non-LTE theory and is applied to these data. The results support the conclusion of other authors that the 304 A line is formed by collisional excitation in the quiet sun, but that photoionization-recombination (p-r) may play a significant role in coronal active regions, and that p-r is important, and may even be predominant, in many flares.

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