Emission line ratios for Fe XXI applicable to the XUV spectra of solar flares

Details Emission line ratios for Fe XXI applicable to the XUV spectra of solar flares Emission line ratios for Fe XXI applicable to the XUV spectra of solar flares

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..149..129k&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 149, no. 1, p. 129-135

Astronomy and Astrophysics

Astronomy

5

Atomic Energy Levels, Atomic Excitations, Electron Impact, Emission Spectra, Iron, Line Spectra, Solar Flares, Ultraviolet Astronomy, Ultraviolet Spectra, High Temperature, Oso-5, Spectrometers

Scientific paper

Electron impact excitation rates for Fe XXI, calculated with the R-matrix code, are used to determine theoretical electron density sensitive emission line ratios involving transitions in the 121-146 A wavelength range. The observed ratios for a solar flare, obtained with a grazing spectrometer on board the OSO-5 satellite, imply electron densities which are consistent, with discrepancies that do not exceed 0.3 dex. In addition, the derived values of Ne are similar to those estimated for the high temperature regions of other solar flares. This provides experimental support for the accuracy of the atomic data adopted in the line ratio calculations.

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