Abstract
Using a linked-parameter technique of level-fitting calculations in a multi configuration basis, a parametric analysis of fine structure (fs) for even-parity levels of V II, involving six configurations, has been performed. This led us to exchange the assignments of two triplets, 3d3(2F)4s c 3F and 3d4 d 3F, reported in earlier analyses as being located at 30,300 cm-1 and 30,600 cm-1, respectively. This is confirmed by experimental hyperfine structure (hfs) A constants, used as fingerprints. Moreover, the current singlet 3d24s2 1D2 position is likely too high. The fs parameters, magnetic Lande g-factors, and the percentage of leading eigenvectors of levels are calculated. We present also predicted singlet, triplet and quintet positions for missing experimental levels up to 100,000 cm-1. The single-electron hfs parameters are determined in their entirety for 51V II for the model space (3d + 4s)4 with good accuracy. For the model space (3d + 4s)4 of 51V II the single-electron hfs parameters are computed; furthermore, our achieved theoretical evaluations of the single-electron hfs parameters, thanks to the use of ab initio calculations, reinforce the validity of these hfs parameter values, deduced from experimental data.
Highlights
The early successful fs analysis of the V II spectrum was due to Meggers and Moore [1]
As only a few lowest energy configuration even-parity levels were available from experimental data, in our previous works regarding the fs of transition metal elements much of our analyses of model spaces were restricted to (3d + 4s)4, (4d + 5s)4 and (5d + 6s
We give for the first time the hfs manybody parameter values with good accuracy for the model space (3d + 4s)4, taking advantage of the accurate work done in [10]
Summary
The early successful fs analysis of the V II spectrum was due to Meggers and Moore [1]. According to their classification, all except two of the terms were known in the configurations 3d34s and 3d4, but 3d24s2 was altogether unknown. Sugar and Corliss compiled the energy levels of vanadium in its 23 stages of ionization, which were analysed from atomic spectra [2]. We propose to fill this absence, as we did previously for many singly ionized atoms: Hf II, Zr II, Ta II, Ti II and Nb II [4]-[8] in an aim to complete previous works and to eliminate erroneous level assignments. The background and motivation of this work should present high interest for astrophysical investigations, very useful in the study of the history of nucleosynthesis, chemically peculiar stars and the sun
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