Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...328..344m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 328, May 1, 1988, p. 344-346. SERC-supported research.
Astronomy and Astrophysics
Astrophysics
15
Abundance, Electron Impact, Emission Spectra, Line Spectra, Plasma Interactions, Solar Spectra, Solar Flares, Solar Maximum Mission, X Ray Spectra
Scientific paper
Recently calculated electron impact collision rates for S xv are used to derive the electron temperature sensitive emission-line ratio G = x + y + z/w, where z is the forbidden 1s21S-1s2s 3S, w is the resonance 1s2 1S-1s2p 1P and x and y, the intercombination 1s2 1S-1s2p 3P2 and 1s2 1S-1s2p 3P1 transitions, respectively. The value of R = z/x + y, the electron density sensitive ratio, was also calculated in its low-density limit (Ro), and both are plotted as functions of the electron temperature. These are found to be in much better agreement with the observed values of Ro and G obtained by the Flat Crystal Spectrometer on the Solar Maximum Mission satellite for the 1980 November 5 flare than are the previous results of Pradhan and Shull (1981). This improvement provides support for the methods and the atomic data adopted in our calculations.
Keenan Francis P.
McCann S. M.
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