A formula for calculating theoretical photoelectron fluxes resulting from the He/+/ 304 A solar spectral line

Details A formula for calculating theoretical photoelectron fluxes resulting from the He/+/ 304 A solar spectral line A formula for calculating theoretical photoelectron fluxes resulting from the He/+/ 304 A solar spectral line

Sep 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981georl...8..995r&link_type=abstract

Geophysical Research Letters, vol. 8, Sept. 1981, p. 995-998.

Physics

8

Electron Flux Density, Flux Quantization, Helium Ions, Photoelectrons, Solar Spectra, Electron Energy, Explorer 55 Satellite, Line Spectra, Positive Ions

Scientific paper

A simplified method for the evaluation of theoretical photoelectron fluxes in the upper atmosphere resulting from the solar radiation at 304 A is presented. The calculation is based on considerations of primary and cascade (secondary) photoelectron production in the two-stream model, where photoelectron transport is described by two electron streams, one moving up and one moving down, and of loss rates due to collisions with neutral gases and thermal electrons. The calculation is illustrated for the case of photoelectrons at an energy of 24.5 eV, and it is noted that the 24.5-eV photoelectron flux may be used to monitor variations in the solar 304 A flux. Theoretical calculations based on various ionization and excitation cross sections of Banks et al. (1974) are shown to be in generally good agreement with AE-E measurements taken between 200 and 235 km, however the use of more recent, larger cross sections leads to photoelectron values a factor of two smaller than observations but in agreement with previous calculations. It is concluded that a final resolution of the photoelectron problem may depend on a reevaluation of the inelastic electron collision cross sections.

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