Transition rates for $3s3p^2\;^4P - 3s3p4s\;^4P^o$ transitions in Al I

Charlotte Froese Fischer; James F. Babb

arXiv:1905.11510·physics.atom-ph·June 5, 2019

Transition rates for $3s3p^2\;^4P - 3s3p4s\;^4P^o$ transitions in Al I

Charlotte Froese Fischer, James F. Babb

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TL;DR

This paper presents relativistic calculations of transition rates between specific energy levels in neutral aluminum, improving agreement with experimental data and reducing previous discrepancies.

Contribution

The study provides new relativistic transition rates for Al I multiplets using GRASP, with improved accuracy over earlier theoretical estimates.

Findings

01

Calculated transition rates are about 10% smaller than observed values.

02

Results reduce discrepancies between theory and experiment.

03

Wave functions obtained for all levels of the multiplets.

Abstract

Fully relativistic calculations have been performed for two multiplets, $3 s 3 p^{2}^{4} P$ and $3 s 3 p 4 s^{4} P^{o}$ , in Al I. Wave functions were obtained for all levels of these multiplets using the GRASP programs. Reported are the E1 transitions rates for all transitions between levels of these multiplets. Transition energies and transition rates are compared with observed values and other theory. Our calculated transition rates are smaller by about 10% than observed rates, reducing a large discrepancy between earlier calculations and experiment.

Tables5

Table 1. Table 1: Convergence of the energy level structure for a valence correlation calculation is compared with observed data ErikssonIsberg1963 ; NIST . All results are in cm -1 .

	$𝒏 = 𝟑$	$𝒏 = 𝟒$	$𝒏 = 𝟓 𝒇$	$𝒏 = 𝟔 𝒇$	Observed
$3 s 3 p^{2} {}^{4}P$ Fine structure
$3 s 3 p^{2} {}^{4}P_{1 / 2}$	0	0	0	0	0.00
$3 s 3 p^{2} {}^{4}P_{3 / 2}$	46	46	45	45	46.55
$3 s 3 p^{2} {}^{4}P_{5 / 2}$	122	121	120	120	122.37
$3 s 3 p 4 s^{4} P^{o}$ Fine structure
$3 s 3 p 4 s {}^{4}P_{1 / 2}^{o}$	0	0	0	0	0.00
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	57	58	56	55	56.10
$3 s 3 p 4 s {}^{4}P_{5 / 2}^{o}$	156	157	153	150	152.08
Multiplet separation
$3 s 3 p 4 s {}^{4}P_{1 / 2}^{o}$ - $3 s 3 p^{2} {}^{4}P_{1 / 2}$	33,213	33,029	32,724	32,696	32,671.05

Table 2. Table 2: Convergence of the energy level structure from a core-valence plus valence correlation calculation is compared with observed data ErikssonIsberg1963 ; NIST . All results are in cm -1 .

	$𝒏 = 𝟓 𝒇$	$𝒏 = 𝟔 𝒇$	$𝒏 = 𝟕 𝒇$	Observed
$3 s 3 p^{2}^{P}$ Fine structure
$3 s 3 p^{2} {}^{4}P_{1 / 2}$	0	0	0	0.00
$3 s 3 p^{2} {}^{4}P_{3 / 2}$	48	45	45	46.55
$3 s 3 p^{2} {}^{4}P_{5 / 2}$	128	120	120	122.37
$3 s 3 p 4 s^{4} P^{o}$ Fine structure
$3 s 3 p 4 s {}^{4}P_{1 / 2}^{o}$	0	0	0	0.00
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	60	56	56	56.10
$3 s 3 p 4 s {}^{4}P_{5 / 2}^{o}$	167	155	153	152.08
Multiplet separation
$3 s 3 p^{2} {}^{4}P_{1 / 2}$ - $3 s 3 p 4 s {}^{4}P_{1 / 2}^{o}$	33,142.58	32,934.21	32,838.33	32,671.05

Table 3. Table 3: Ab initio electric dipole (E1) transition data for the 3 s 3 p 2 P 4 3 𝑠 3 superscript 𝑝 2 superscript 𝑃 4 3s3p^{2}\;{}^{4}P to 3 s 3 p 4 s 4 P o 3 𝑠 3 𝑝 4 superscript 𝑠 4 superscript 𝑃 𝑜 3s3p4s\;^{4}P^{o} transition computed in the length form from valence correlation results.

Upper	Lower	$𝚫 𝑬$ (cm^-1)	$𝝀$ (nm)	$𝑨$ ( $𝛍$ s^-1)	$𝒈 𝒇$	$𝒅 𝑻$
$3 s 3 p 4 s {}^{4}P_{1 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{1 / 2}$	32,696	305.84220	29.93	0.0840	0.016
$3 s 3 p 4 s {}^{4}P_{1 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{3 / 2}$	32,650	306.27027	149.01	0.4191	0.017
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{1 / 2}$	32,752	305.32421	75.11	0.4199	0.014
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{3 / 2}$	32,706	305.75074	23.89	0.1339	0.015
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{5 / 2}$	32,631	306.44982	80.43	0.4529	0.017
$3 s 3 p 4 s {}^{4}P_{5 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{3 / 2}$	32,801	304.86634	54.37	0.4546	0.014
$3 s 3 p 4 s {}^{4}P_{5 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{5 / 2}$	32,726	305.56128	125.94	1.0577	0.015

Table 4. Table 4: Ab initio electric dipole (E1) transition data for the 3 s 3 p 2 P 4 3 𝑠 3 superscript 𝑝 2 superscript 𝑃 4 3s3p^{2}\;{}^{4}P to 3 s 3 p 4 s 4 P o 3 𝑠 3 𝑝 4 superscript 𝑠 4 superscript 𝑃 𝑜 3s3p4s\;^{4}P^{o} transition computed in the length form from valence and core-valence results.

$n = 5 f$
Upper	Lower	$𝚫 𝑬$ (cm^-1)	$𝝀$ (nm)	$𝑨$ ( $𝛍$ s^-1)	$𝒈 𝒇$	$𝒅 𝑻$
$3 s 3 p 4 s {}^{4}P_{1 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{1 / 2}$	33,142	301.727	29.76	0.0812	0.004
$3 s 3 p 4 s {}^{4}P_{1 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{3 / 2}$	33,093	302.170	148.19	0.4057	0.006
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{1 / 2}$	33,203	301.173	74.72	0.4064	0.001
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{3 / 2}$	33,154	301.615	23.88	0.1303	0.003
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{5 / 2}$	33,075	302.341	79.91	0.4380	0.008
$3 s 3 p 4 s {}^{4}P_{5 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{3 / 2}$	33,261	300.652	53.83	0.4377	0.001
$3 s 3 p 4 s {}^{4}P_{5 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{5 / 2}$	33,181	301.373	125.12	1.0223	0.003
$n = 7 f$
$3 s 3 p 4 s {}^{4}P_{1 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{1 / 2}$	32,838	304.522	28.51	0.0793	0.051
$3 s 3 p 4 s {}^{4}P_{1 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{3 / 2}$	32,792	304.947	141.94	0.3958	0.053
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{1 / 2}$	32,894	304.003	71.57	0.3966	0.049
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{3 / 2}$	32,848	304.426	22.85	0.1270	0.050
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{5 / 2}$	32,773	305.120	76.55	0.4274	0.055
$3 s 3 p 4 s {}^{4}P_{5 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{3 / 2}$	32,946	303.523	51.61	0.4277	0.047
$3 s 3 p 4 s {}^{4}P_{5 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{5 / 2}$	32,871	304.213	119.86	0.9979	0.050

Table 5. Table 5: Comparison of the transition rates computed from valence correlation calculations (present) and observed wavelengths (in a vacuum) from NIST ErikssonIsberg1963 ; NIST with observed rates from Hermann et al. Hermann and values reported by Kurucz and Peytremann Kurucz

Upper	Lower	$𝝀$ (nm)		$𝑨$ ( $𝛍$ s^-1)
		NIST	Present	Present	Hermann	Kurucz
$3 s 3 p 4 s {}^{4}P_{1 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{1 / 2}$	305.9924	305.8422	29.89	34.	18.3
$3 s 3 p 4 s {}^{4}P_{1 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{3 / 2}$	306.4290	306.2703	148.80	160.	89.2
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{1 / 2}$	305.4679	305.3242	74.99	78.	44.9
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{3 / 2}$	305.9029	305.7507	23.85	28.	14.2
$3 s 3 p 4 s {}^{4}P_{3 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{5 / 2}$	306.6144	306.4498	80.32	90.	47.7
$3 s 3 p 4 s {}^{4}P_{5 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{3 / 2}$	305.0073	304.8663	54.28	59.	32.1
$3 s 3 p 4 s {}^{4}P_{5 / 2}^{o}$	$3 s 3 p^{2} {}^{4}P_{5 / 2}$	305.7144	305.5613	125.75	140.	75.0

Equations10

Ψ (γ P J M_{J}) = j = 1 \sum M c_{j} Φ (γ_{j} P J M_{J}) .

Ψ (γ P J M_{J}) = j = 1 \sum M c_{j} Φ (γ_{j} P J M_{J}) .

ψ_{nκ, m} (r) = \frac{1}{r} (P_{nκ} (r) χ_{κ, m} (θ, φ)  Q_{nκ} (r) χ_{- κ, m} (θ, φ)),

ψ_{nκ, m} (r) = \frac{1}{r} (P_{nκ} (r) χ_{κ, m} (θ, φ)  Q_{nκ} (r) χ_{- κ, m} (θ, φ)),

\displaystyle w_{a}\left[\begin{array}[]{c c}V(a;r)&-c\left[\frac{d}{dr}-\frac{\kappa_{a}}{r}\right]\\ \\ c\left[\frac{d}{dr}+\frac{\kappa_{a}}{r}\right]&V(a;r)-2c^{2}\end{array}\right]\left[\begin{array}[]{c}P_{a}(r)\\ Q_{a}(r)\end{array}\right]=\sum_{b}\epsilon_{ab}\;\delta_{\kappa_{a}\kappa_{b}}\left[\begin{array}[]{c}P_{b}(r)\\ Q_{b}(r)\end{array}\right],

\displaystyle w_{a}\left[\begin{array}[]{c c}V(a;r)&-c\left[\frac{d}{dr}-\frac{\kappa_{a}}{r}\right]\\ \\ c\left[\frac{d}{dr}+\frac{\kappa_{a}}{r}\right]&V(a;r)-2c^{2}\end{array}\right]\left[\begin{array}[]{c}P_{a}(r)\\ Q_{a}(r)\end{array}\right]=\sum_{b}\epsilon_{ab}\;\delta_{\kappa_{a}\kappa_{b}}\left[\begin{array}[]{c}P_{b}(r)\\ Q_{b}(r)\end{array}\right],

H c = E c,

H c = E c,

H_{ij} = ⟨ Φ (γ_{i} P J M_{J}) ∣ H ∣Φ (γ_{j} P J M_{J})⟩ .

H_{ij} = ⟨ Φ (γ_{i} P J M_{J}) ∣ H ∣Φ (γ_{j} P J M_{J})⟩ .

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Full text

Abstract

Fully relativistic calculations have been performed for two multiplets, $3s3p^{2}\;{}^{4}P$ and $3s3p4s\;^{4}P^{o}$ , in Al i. Wave functions were obtained for all levels of these multiplets using the grasp programs. Reported are the E1 transitions rates for all transitions between levels of these multiplets. Transition energies and transition rates are compared with observed values and other theory. Our calculated transition rates are smaller by about 10% than observed rates, reducing a large discrepancy between earlier calculations and experiments.

keywords:

atomic spectra; energy levels;transition probabilities; wavelengths; aluminum

\pubvolume

7 \issuenum1 \articlenumber54

\historyReceived: 1 May 2019; Accepted: 26 May 2019; Published: 4 June 2019 \TitleTransition Rates for $3s3p^{2}\;{}^{4}P-3s3p4s\;^{4}P^{o}$ Transitions in Al i

\AuthorCharlotte Froese Fischer 1\orcidA and James F. Babb 2\orcidB

\corresCorrespondence: [email protected]; Tel.: +1-604-225-5147. [email protected]; Tel.: +1-617-496-7612

1 Introduction

Atomic spectra are of vital importance as plasma diagnostics and reliable wavelengths and transition probabilities are essential for applications. Recently, Hermann et al. Hermann deduced transition probabilities between the fine structure lines connecting the $3s3p^{2}\;{}^{4}P$ and $3s3p^{2}\;{}^{4}P^{o}$ multiplets from emission coefficients measured in laser ablation of aluminum in argon. The transition probabilities obtained were roughly a factor of two larger than those listed in the semi-empirical calculations of Kurucz and Peytremann Kurucz , and no other values were found in existing tabulations. The fine structure lines connecting the $3s3p^{2}\;{}^{4}P$ and $3s3p^{2}\;{}^{4}P^{o}$ multiplets occur in the same general wavelength region (305–310 nm) and with comparable strength as the well-studied (see ref-Papoulia and the references therein) fine structure lines connecting the $3s^{2}3p\;^{2}P$ and $3s^{2}3d\;^{2}D$ multiplets, making the discrepancy of concern for applications in the UV wavelengths.

Multiconfiguration Dirac–Hartree–Fock (MCDHF) and relativistic configuration interaction (RCI) calculations have been performed by Papoulia et al. ref-Papoulia for 28 states in neutral Al. The configurations of interest were $3s^{2}nl$ for $n=3,4,5$ with $l$ = 0–4, as well as $3s3p^{2}$ and $3s^{2}6l$ for $l=0,1,2$ . Lifetimes and transition data for radiative electric dipole (E1) transitions were reported. There was a significant improvement in accuracy, in particular for the more complex system of neutral Al i, which may prove useful for astrophysical applications to Al abundance determinations in stars. Omitted were the levels of the $3s3p4s\;^{4}P^{o}$ multiplet, which lies above the first $3s^{2}$ ionization limit ErikssonIsberg1963 .

This paper reports transition rates for all E1 transitions between the $3s3p^{2}\;{}^{4}P$ and $3s3p4s\;^{4}P^{o}$ multiplets using the variational multiconfiguration Dirac–Hartree–Fock (MCDHF) method review , as implemented in the grasp programs GRASP . The accuracy of the results is based on the accuracy of the theoretically-predicted transition energies compared with available measurements, as well as the agreement between length and velocity rates.

2 Underlying Theory

In the MCDHF method review , the wave function $\Psi({\gamma}PJM_{J})$ for a state labeled ${\gamma}PJM_{J}$ , where $J$ and $M_{J}$ are the angular quantum numbers and $P$ the parity, is expanded in antisymmetrized and coupled configuration state functions (CSFs):

[TABLE]

The labels $\{\gamma_{j}\}$ denote other appropriate information about the CSFs, such as orbital occupancy and the coupling scheme. The CSFs are built from products of one-electron orbitals, having the general form:

[TABLE]

where $\chi_{\pm\kappa,m}(\theta,\varphi)$ are two-component spin-angular functions. The expansion coefficients and the radial functions are determined iteratively. In the present work, the Dirac–Coulomb Hamiltonian ${\cal H}_{DC}$ was used review , which included a correction for the finite size of the nucleus.

The radial functions $\{P_{n\kappa}(r),Q_{n\kappa}(r)\}$ were determined numerically as solutions of differential equations,

[TABLE]

where $V(a;r)=V_{nuc}(r)+Y(a;r)+\bar{X}(a;r)$ is a potential consisting of nuclear, direct, and exchange contributions arising from both diagonal and off-diagonal $\langle\Phi_{\alpha}|{\cal H}_{DC}|\Phi_{\beta}\rangle$ matrix elements review .

For a given set of radial functions, expansion coefficients ${\bf c}=(c_{1},\ldots,c_{M})^{t}$ were obtained as solutions to the configuration interaction (CI) problem,

[TABLE]

where ${\bf H}$ is the CI matrix of dimension $M\times M$ with elements

[TABLE]

Once self-consistent solutions have been obtained—sometimes referred to as the relativistic MCDHF or RMCDHF phase—an RCI calculation was performed using an extended Hamiltonian that included the transverse photon (Breit) and QED corrections. Wave functions from the latter Hamiltonian were used to compute the E1 transitions rates.

3 Systematic Procedures

Systematic procedures were used in which the orbital set used for defining the wave function expansion increased systematically within a correlation model.

The states of Al consist of a neon-like ( $1s^{2}2s^{2}2p^{6}$ ) core and three valence electrons. Wave function expansions were obtained from single- and double- (SD) excitations from a multireference (MR) set that interacted significantly with the CSFs of interest. For the even multiplet, the MR set included the CSFs from $3s3p^{2}$ , $3s3d^{2}$ , and $3p^{2}3d$ configurations and for the odd multiplet, CSFs from $3s3p4s$ , $3p3d4s$ , $3p^{2}4p$ , and $3s3d4p$ . Because the odd multiplet was above the first ionization limit, all $3s^{2}nl$ CSFs were removed. In this paper, the orbital sets that define the set of excitations were classified according to the largest $nl$ of the orbital set when the latter were ordered globally by $n$ (the principal quantum number) and within $n$ by $l$ (the orbital quantum number). Thus, an $n=3$ orbital set includes all orbitals up to $3s,3p,3d$ and all $n=5f$ orbitals up to $5s,5p,5d,5f$ ( $5g$ not included).

Our first model was the valence correlation (VV) model, in which all excitations involved only valence electrons. $n=3$ calculations were performed for an average energy functional of the lowest even parity $J=1/2,3/2,5/2$ states. This calculation defined the core orbitals for all subsequent calculations. The $n=4,5f,6f$ calculations each varied only the new orbitals. For the odd multiplet, the first calculation had orbitals up to $4s$ , $4p$ , and $3d$ , but is still referred to as an $n=3$ calculation in this paper, with remaining sets being the regular $n=4,5f,6f$ orbital sets. Table 1 shows the convergence of the fine-structure of the two multiplets and their separation.

The results of the converged valence correlation calculations, when compared with observation, suggest that the energy structure is not significantly affected by the core-valence (CV) that accounts for the polarization for the core. To confirm this conclusion, calculations were performed in which SD excitations included a single excitation from the $2p$ -shell along with a single excitation of a valence electron. Wave function expansions were considerably larger and convergence a bit slower. Table 2 shows the convergence of the energy structure. The fine structure of the odd multiplet increased slightly and was in somewhat better agreement with the data from observation. At the same time, the transition energy for ${}^{4}P_{1/2}-^{4}P^{o}_{1/2}$ for an $n=7f$ calculation was not in as good agreement with observed as the $n=6f$ valence correlation calculation reported in Table 1.

4 Results

The wave functions from RCI expansions, determined using the Dirac–Coulomb–Breit-QED Hamiltonian, were used to compute the E1 transition rates for all transitions between these two multiplets. Table 3 reports the transition energy $\Delta E$ (cm*-1*), the wavelength $\lambda$ (nm) in a vacuum, $A$ ( $\upmu$ s*-1*), and $gf$ , in the length form for calculations of Table 1. Furthermore included is an indicator of accuracy $dT=(A_{l}-A_{v})/\mathrm{max}(A_{l},A_{v})$ , where $A_{l}$ and $A_{v}$ are transition rates from length and velocity forms, respectively. The average discrepancy between the two forms was 1.5%, and in all cases, the velocity form had a larger value than the length form.

The effect of core-valence is shown in Table 4 where results are reported both for the $n=5f$ and $n=7f$ calculation. The former was included because of the remarkable agreement in length and velocity forms, yet the transition energy (as shown in Table 2) was not in as good agreement with the observed as before. Since the transition rate is proportional to $(\Delta E)^{3}$ , correcting the transition rate for this factor would introduce a 4.0% reduction. Indeed, the $n=7f$ transition rates were smaller with the transition energy more accurate, but length and velocity were not in as good agreement.

In summary, valence correlation predicted the best transition energy and the best agreement in length and velocity for accurate transition energy.

5 Summary and Conclusions

Table 5 compares the predicted transition rates (based on observed transition energies or wavelengths in a vacuum, rather than computed transition energies as in Table 4), with values derived from observations by Hermann et al. Hermann and the values reported by Kurucz and Peytremann Kurucz . The latter used a semi-empirical approach in which Slater parameters were determined empirically from observed energy levels and transition probabilities calculated by the use of scaled Thomas–Fermi–Dirac wave functions. As seen in Table 5, the present predicted transition rates are about 10% smaller than observed values, whereas the Kurucz and Peytremann values are about a half those of the observed rates. Thus, the discrepancy between theory and experiment has been reduced significantly.

\authorcontributions

The authors C.F.F. and J.F.B. contributed jointly to conceptualization, methodology, validation, formal analysis, writing–original draft preparation, and writing–review and editing.

\funding

This research was funded by Canada NSERC Discovery Grant 2017-03851 (CFF) and US NSF Grant No. PHY-1607396 (JFB). The APC was funded by MDPI.

Acknowledgements.

The authors (CFF and JB) acknowledge support, respectively, from the Canada NSERC Discovery Grant 2017-03851 and from ITAMP , which is supported in part by Grant No. PHY-1607396 from the NSF to Harvard University and the Smithsonian Astrophysical Observatory. \conflictsofinterestThe authors declare no conflict of interest. The funders had no role in the design of the study; in the collection, analyses, or interpretation of data; in the writing of the manuscript, or in the decision to publish the results. \reftitleReferences

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