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Theoretical emission line strengths for Ov compared to EUV solar observations

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Abstract

RecentR-matrix calculations of electron impact excitation rates in Ov are used to derive the emission line intensity ratios (in energy units)

$$\begin{gathered} R_1 = I(2s2p^{ 3} P - 2p^{2 3} P)/I(2s^{2 1} S_0 - 2s2p^{ 1} P_1 ) = I(761.1\mathop A\limits^ \circ )/I(629.7\mathop A\limits^ \circ ), \hfill \\ R_2 = I(2s^{2 1} S_0 - 2s2p^{ 3} P_1 )/I(2s^{2 1} S_0 - 2s2p^{ 1} P_1 ) = I(1218.4\mathop A\limits^ \circ )/I(629.7\mathop A\limits^ \circ ), \hfill \\ \end{gathered} $$

and

$$R_3 = I(2s2p^{ 1} P_1 - 2p^{2 1} S_0 )/I(2s^{2 1} S_0 - 2s2p^{ 1} P_1 ) = I(774.5\mathop A\limits^ \circ )/I(629.7\mathop A\limits^ \circ )$$

as a function of electron temperature (T e) and density (N e). These results are presented as plots ofR 1 vsR 2, andR 1 vsR 3, which should allowboth N e andT e to be deduced for the Ov line emitting region of a plasma. Electron densities derived from the (R 1,R 2) and (R 1,R 3) diagrams in conjunction with observational data for several solar features obtained with the Harvard S-055 spectrometer on boardSkylab are found to be compatible, and in good agreement with values ofN e estimated from line ratios in species formed at similar electron temperatures to Ov. In addition, values ofT e determined from (R 1,R 2) and (R 1,R 3) are generally close to that expected theoretically. These results provide experimental support for the accuracy of the diagnostic calculations presented in this paper, and hence the atomic data used in their derivation.

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Authors and Affiliations

  1. Department of Pure and Applied Physics, The Queen's University of Belfast, BT 7 1NN, Belfast, N. Ireland

    F. P. Keenan & G. A. Warren

  2. Armagh Observatory, BT61 9DG, Armagh, N. Ireland

    J. G. Doyle

  3. Department of Applied Mathematics and Theoretical Physics, The Queen's University of Belfast, BT 7 1NN, Belfast, N. Ireland

    K. A. Berrington & A. E. Kingston

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  1. F. P. Keenan
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  2. G. A. Warren
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  4. K. A. Berrington
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  5. A. E. Kingston
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Keenan, F.P., Warren, G.A., Doyle, J.G. et al. Theoretical emission line strengths for Ov compared to EUV solar observations. Sol Phys 150, 61–70 (1994). https://doi.org/10.1007/BF00712876

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  • DOI: https://doi.org/10.1007/BF00712876

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