Energy Levels and Radiative Rates for Transitions in F-like Sc XIII and Ne-like Sc XII and Y XXX

Abstract

Abstract:Energy levels, radiative rates and lifetimes are reported for F-like Sc XIII and Ne-like Sc XII and Y XXX for which the general-purpose relativistic atomic structure package (GRASP) has been adopted. For all three ions, limited data exist in the literature but comparisons have been made wherever possible to assess the accuracy of the calculations. In the present work, the lowest 102, 125 and 139 levels have been considered for the respective ions. Additionally, calculations have also been performed with the flexible atomic code (FAC) to (particularly) confirm the accuracy of energy levels.

Radiative rates for E1, E2, M1, and M2 transitions in F-like ions with 12 ≤ Z ≤ 23

“…Combined with our earlier results [2][3][4][5][6][7][8]18], along with those of Si et al [9] and Li et al [10], the present work completes data for all F-like ions with Z ≤ 74. These works include a larger number of levels than generally available in the literature, are comparatively more accurate, and hence can be confidently and reliably applied in the diagnostics and modelling of a variety of plasmas, including astrophysical and fusion.…”

“…Also included in these tables are the results from the MCHF calculations of Froese Fischer and Tachiev [16], but only for the lowest 60 levels. It may be noted that the results for Sc XIII are not included here (or in subsequent tables), because these have already been discussed in a separate paper [18]. Finally, as already stated and demonstrated in earlier works, with the inclusion of same CI there are no appreciable discrepancies in energies (for most of the levels) obtained from the GRASP and FAC codes.…”

Comment on “Energy levels, oscillator strengths, and transition probabilities for sulfur-like scandium, Sc VI” by El-Maaref et al. [Indian J. Phys. 91 1029 (2017)]

“…Scandium (Sc) belongs to the group of rare earth elements and hence atomic data for its ions are useful for the studies of fusion plasmas [1]. It is also an important element for the studies of astrophysical plasmas, as discussed by Pryce [2], and is a key element for understanding Am stars, as demonstrated by LeBlanc and Alecian [3].…”