Abstract
Equilibrium population of Fexiv levels in coronal conditions was calculated including configurations 3s 23p, 3s3p 2, 3s 23d, 3p 3, 3s3p3d, 3s 24s, 3s 24p, 3s 24d, 3s 24f. Relative populations of selected levels are given in Table VII. Figure 1 shows the dependence of relative intensities of the strongest lines on electron density. Certain line ratios can be used for the determination of N e .E.g., at T=2 × 106 K and with a dilution factor 0.4, the intensity ratio of λ211.3 and λ219.0 changes by a factor of 65 if N e increases from 107 to 1011 (Table VIII). Cascades from the 3s3p3d and 3p 3 configurations are important in the population of some levels of 3s3p 2 (Table VI). A possibility of identification of additional lines in the solar spectrum is indicated.
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NAS-NRC Resident Research Associate.
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Blaha, M. Theoretical intensities of Fexiv in the solar EUV spectrum. Sol Phys 17, 99–116 (1971). https://doi.org/10.1007/BF00152865
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DOI: https://doi.org/10.1007/BF00152865