Fe XVIII emission-line intensities in the sun

Details Fe XVIII emission-line intensities in the sun Fe XVIII emission-line intensities in the sun

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...385..378m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 385, Jan. 20, 1992, p. 378-380. Research supported by Aerospace Corp., Nuff

Astronomy and Astrophysics

Astrophysics

8

Electron States, Emission Spectra, Iron, Metallicity, Solar Spectra, Solar X-Rays, Atomic Energy Levels, Electron Impact, Oscillator Strengths, Solar Corona

Scientific paper

Recently calculated electron-impact excitation rates among the 2s2 2p5, 2s2p6, and 2s2 2p4nl levels of Fe XVIII are used to derive theoretical emission-line ratios applicable to solar X-ray spectra. Oscillator strengths for all levels with n of less than or equal to 3 are used to take cascade involving the levels fully into account. Overall, the agreement between the theory and spectra measured by crystal spectrometers aboard the OV 1-17, P78-1, and SMM satellites is good. The effects of cascade from levels for which n is at least 4 are small, at least for the strongest lines. The labor required to take into account these higher levels is not justified by the current discrepancies between theory and observation.

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