Improved theoretical line ratios for C III in the sun

Details Improved theoretical line ratios for C III in the sun Improved theoretical line ratios for C III in the sun

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...99...25k&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 99, Sept. 1985, p. 25-30. SERC-supported research.

Mathematics

26

Carbon, Line Spectra, Solar Spectra, Matrices (Mathematics), Transition Probabilities

Scientific paper

Berrington's (1985) 12-state R-matrix calculations of electron excitation rates are used to derive level populations applicable to the solar transition region. The close coupled impact parameter results of Doyle et al. (1980) are used, together with Einstein A-coefficients for C III obtained by Nussbaumer and Storey (1978). Level populations for C III were derived on the basis of the statistical equilibrium code of Dufton (1977). The R and R(2) line ratios deduced from the data, in conjunction with the relevant transition probabilities, are noted to be in much better agreement with the observed, quiet sun values than with those determined from the level population calculations of Keenan et al. (1984).

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