Theoretical intensities of Fexiv in the solar EUV spectrum

Abstract

Equilibrium population of Fexiv levels in coronal conditions was calculated including configurations 3s23p, 3s3p2, 3s23d, 3p3, 3s3p3d, 3s24s, 3s24p, 3s24d, 3s24f. 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 Ne.E.g., at T=2 × 106K and with a dilution factor 0.4, the intensity ratio of λ211.3 and λ219.0 changes by a factor of 65 if Neincreases from 107 to 1011 (Table VIII). Cascades from the 3s3p3d and 3p3 configurations are important in the population of some levels of 3s3p2 (Table VI). A possibility of identification of additional lines in the solar spectrum is indicated.