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The l(1)S-n(1)P/1(1)S-2(1)P emission-line ratios in O VII as temperature diagnostics for solar flares and active regions
Keenan, F. P.; Kingston, A. E.; McKenzie, D. L.
AA(Belfast, Queen's University, Belfast, Northern Ireland), AB(Belfast, Queen's University, Belfast, Northern Ireland), AC(Aerospace Corp., Space Sciences Laboratory, Los Angeles, CA)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 291, April 15, 1985, p. 855-857. Research supported by the Science and Engineering Research Council and Aerospace Corp. (ApJ Homepage)
Publication Date:
Solar Physics
NASA/STI Keywords:
Emission Spectra, Oxygen Ions, Solar Activity, Solar Flares, Solar Spectra, Electron Energy, Radiative Recombination
Bibliographic Code:


Recent R-matrix calculations of O VII electron excitation rates by Tayal and Kingston are used to determine the theoretical emission-line ratios R1 = I(1s2 1S-ls3p1P)/I(1s2 1S-ls2p1P) and R2 = I(1s2 1S-ls4p1P)/ I(1s2 1S-ls2p1P). These ratios are found to vary by factors of 3.3 and 4.9, respectively, between Te = 6 x 1O5 and 2 x 106 K. However, G = [I(1s2 1S-1s2s3S) + I(1s2 1S-ls2p3P)]/I(1s2 1S-ls2p1P), a commonly used temperature diagnostic for He-like ions, only varies by a factor of 1.8. Electron temperatures derived using observed values of R1 and R2 from P78-1 satellite spectra of solar flares and active regions are in good agreement and compare favorably with those deduced from G.

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