Transition Parameters for Doubly Ionized Lanthanum

The transition parameters such as the wavelengths, weighted oscillator strengths, and transition probabilities (or rates) for the nd (n = 5−9)−nf (n = 4−8), nd (n = 5−9)−np (n = 6−9), np (n = 6−9)−ns (n = 6−10), and ng (n = 5−8)−nf (n = 4−8) electric dipole (E1) transitions of doubly ionized lanthanum (La III,Z = 57) have been calculated using the relativistic Hartree-Fock (HFR) method. In this method, configuration interaction and relativistic effects have been included in the computations combined with a least squares fitting of the Hamiltonian eigenvalues to the observed energy levels. We have compared the results obtained from this work with the previously available calculations and experiments in literature. We have also reported new transitions with the weighted transition probabilities greater than or equal to 105.


Introduction
The radiative properties of the lanthanides and their ions have been rather little considered.This can be explained by the fact that these atoms or ions are characterized by complex electronic structures with an unfilled 4f subshell, which makes the calculations very difficult, and that the laboratory analyses are still extremely fragmentary or even missing for many ions.Owing to the importance of rare earth elements in astrophysics, especially in relation to nucleosynthesis and star formation (notably the lanthanides in chemically peculiar (CP) stars) [7], there is a growing need for accurate spectroscopic data, that is, wavelengths, radiative transition rates, oscillator strengths, branching fractions, radiative lifetimes, hyperfine structure, and isotope shift data for lanthanide atoms and ions.
The lanthanum atom is the first member of the rare earth elements.Doubly ionized lanthanum (La III) is characterized by a simple atomic structure with core [Xe] and only one outer electron.There is substantial spectroscopic literature concerning La III, though less than the neutral or singly ionized species.The available theoretical and experimental works on energy levels, radiative lifetimes, and transition parameters for La III can be found in the literature [1-3, 5, 6, 8-13].These works were reported in our previous work in detail [14].
Up till now the wavelengths, oscillator strengths, and transition probabilities available for La III were obtained by experimental, semiempirical, or pure theoretical approaches.Sixty-five spectral lines of La III in the 2000-12000 Å interval were reported by Odabasi [2].Sugar and Kaufman [13] observed forty-five La III spectral lines in the interval from 700 to 2000 Å. Johansson and Litzén [5] recorded wavelengths of 5d-4f lines of La III.Relativistic single-configuration Hartree-Fock oscillator strengths for 6s-6p transitions in La III were reported by Migdalek and Baylis [4].Migdalek and Wyrozumska [3] have calculated oscillator strengths obtained using the relativistic model-potential approach in there different versions: a model-potential without valencecore electron exchange but with core-polarization included (RMP + CP), with semiclassical exchange and core-polarization (RMP + SCE + CP), and with empirically adjusted exchange and core-polarization (RMP + EX + CP) for the 6s-6p, 5d-6p, 5d-4f, 5d-5f, 5d-6f, 6p-6d, and 6p-7d transition arrays.The single-configuration relativistic Hartree-Fock ionization potentials of La III were computed by Migdalek and Bojara [9].Biémont et al. [1] have performed oscillator strengths and transition probabilities in La III by relativistic Hartree-Fock method with core-polarization.

Calculation Method
An electromagnetic transition between two states is characterized by the angular momentum and the parity of the corresponding photon.If the emitted or absorbed photon has angular momentum k and parity π = (−1) k then, the transition is an electric multipole transition (Ek).However, if the photon has parity π = (−1) k+1 the transition is a magnetic multipole transition (Mk).
According to HFR method [16], the total transition probability from a state γ J M to all states M levels of γJ is given by and absorption oscillator strength is given by where, σ = [(E j −E i )/hc] has units of kaysers (cm −1 ) and S = | γJ P (1) γ J | 2 is the electric dipole line strength in atomic units of e 2 a 2 0 .The strongest transition rate (or probability) is electric dipole (E1) radiation.For this reason, the E1 transitions are understood as being "allowed", whereas highorder transitions are understood as being "forbidden".
In HFR method, for an N electron atom of nuclear charge Z 0 , the Hamiltonian is expanded as in atomic units, with r i the distance of the ith electron from the nucleus and r i j is the spin-orbit term, with α being the fine structure constant and V the mean potential field due to the nucleus and other electrons.
In this method, one calculates single-configuration radial functions for a spherically symmetrised atom (center-ofgravity energy of the configuration) based on Hartree-Fock method.The radial wave functions are also used to obtain the atom's total energy (E av ) including approximate relativistic and correlation energy corrections.Relativistic terms in the potential function give approximate relativistic corrections to the radial functions, as well as improved relativistic energy corrections in heavy atoms.In addition, a correlation term is included to make the potential function more negative, thereby helping to bind negative ions.These radial functions are also used to calculate Coulomb integrals F k and G k and spin-orbit integrals ζ nl .After radial functions have been obtained based on Hartree-Fock model, the wave function |γJM of the M sublevel of a level labeled γJ is expressed in terms of LS basis states |αLSJM by the formula If determinant wave functions are used for the atom, the total binding energy is given by where E i k is the kinetic energy, E i n is the electron-nuclear Coulomb energy, and E i j is the Coulomb interaction energy    between electrons i and j averaged over all possible magnetic quantum numbers.In this method, relativistic corrections have been limited to calculations to the mass-velocity and the Darwin corrections by using the relativistic correction to total binding energy.The total binding energy can be given in by formulas (7.57), (7.58), and (7.59) in [16].
Electron correlation effects and relativistic effects play an important role in the spectra of heavy elements.To accurately predict the radiative atomic properties for heavy atoms such as La III, complex configuration interactions and relativistic effects must be considered simultaneously.Although Cowan's approach is based on Schrödinger's equation, it includes the most important relativistic effects like massvelocity corrections and Darwin contributions.Also, for complex atoms, it is important to allow for spin-orbit interaction, which represents the magnetic interaction energy between electron's spin magnetic moment and the magnetic field that the electron sees due to its orbital motion through the electric field of the nucleus.These contributions are considered as perturbations.Thus, to solve the Schrödinger equation with this Hamiltonian, we define a new angular momentum operator in an intermediate coupling scheme.
In calculations, the eigenvalues of Hamiltonian were optimized to the observed energy levels via a least-squares fitting procedure using experimentally determined energy levels, specifically all of the levels from the NIST compilation [28].The scaling factors of the Slater parameters (F k and G k ) and of configuration interaction integrals (R k ), not optimized in the least-squares fitting, were chosen equal to 0.85, while the spin-orbit parameters were left at their initial values.This low value of the scaling factors has been suggested by Cowan for neutral heavy elements [15,16].
We obtained 7785 and 4278 possible E1 transitions between odd-and even-parity levels in the calculations A and B, respectively.The results obtained are in excellent agreement with those of other works except some transitions.For some transitions, although the agreement is less in the weighted oscillator strengths and the weighted transition probabilities, it is very good in the wavelengths.Most of results related to low-lying levels obtained from this work are in agreement with literature [1][2][3][4][5][6].The differences between our HFR results and other works for gf and gA ki have been found in the 0-10% range for the transitions np (n = 6-8)-ns (n = 6-10), nd (n = 6-9), in the 0.5-9% range for the transitions nd (n = 6, 7)-nf (n = 5-8), np (n = 7-9), and in the 1.5-20% range for the transitions nf (n = 5-8)-nd (n = 7-9), ng (n = 5-8).But the agreement is less in the weighted oscillator strengths and the weighted transition probabilities for 5d and 4f transitions.In fact, except the transitions 6p  [1].Except the transitions 5d-9p, 4f-7g, 8g, 8s-9p, and 4f-6d, we found also the values 1.084 (in calculation A) and 1.126 (in calculation B) for the mean ratio gA ki (this work)/gA ki [1].The transition results obtained from the calculation A agree with other works.This calculation includes core correlation (including excitation from 5p shell in core).These results obtained from HFR calculations may be better in case that the increasing number of configurations including the excitations from core.It is noted that there are no exist the works, especially experimental, on La III recently in available literature.A detailed comparison needs new experimental works.Most of our results are excellent in agreement, expect the transition results to 4f and 5d levels (for gf and gA ki results), generally.It is well known that these levels interact strongly with core.
In conclusion, the main purpose of this paper was to perform HFR calculations for obtaining the description of La III spectrum.Accurate atomic structure data is an essential ingredient for a wide range of research fields.Areas from plasma research applications in nuclear fusion to lighting research, as well as astrophysics and cosmology, depend on such data.In spectrum synthesis works, particularly for CP stars, accurate data for transition probabilities (rates) and oscillator strengths for lanthanide atoms are needed to establish reliable abundances for these species.The agreement is excellent, especially for wavelengths, when our HFR results are compared with other available works in literature for the radiative transitions for La III.So, we may mention that new results presented in Table 2 for the transitions between some highly levels in this work are also reliable.There are a few experimental or theoretical radiative transition data for La III in literature.Consequently, we hope that our results, especially the new results in Table 2, which are obtained using the HFR method will be useful for research fields, technological applications, and other works in the future for La III spectra.