Oscillator Strengths and Lifetimes for the P XIII Spectrum

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Spectral Analysis Reviews, 016,, 1-10 Published Online January 016 in SciRes. http://www.scirp.org/journal/sar http://dx.doi.org/10.36/sar.016.1001 Oscillator Strengths and Lifetimes for the P XIII Spectrum A.

Luna Universidade Estadual de Santa Cruz, DCET, Ilhéus, Brazil Received 3 May 016; accepted 17 July 016; published 0 July 016 Copyright 016 by authors and Scientific Research Publishing Inc.

1 Spectral Analysis Reviews, 016,, 1-10 Published Online January 016 in SciRes. Oscillator Strengths and Lifetimes for the P XIII Spectrum A. J. Mania, F. R. T. Luna Universidade Estadual de Santa Cruz, DCET, Ilhéus, Brazil Received 3 May 016; accepted 17 July 016; published 0 July 016 Copyright 016 by authors and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY). Abstract The P XIII spectrum has been analyzed by several authors using different light sources. The semiempirical oscillator strengths (gf) and the lifetimes presented in this work for all known P XIII spectral lines and energy levels were carried out in a multi-configuration Hartree-Fock relativistic (HFR) approach. In this calculation, the electrostatic parameters were optimized by a leastsquares procedure in order to improve the adjustment of theoretical to experimental energy levels. The method produces gf-values that are in agreement with intensity observations and lifetime values closer to the experimental ones. Keywords P XIII Spectrum, Atomic Transitions, Energy Levels, Oscillator Strengths, Lifetimes 1. Introduction The ground state configuration of twelve times ionized phosphorus, P XIII is 1s s with the term S 1/ being this spectrum a member of the Li-like isoelectronic sequence with a complete core plus a single-electron valence shell. The ionization limit for this ion is estimated as being,93,000 ± 600 (611.7± 0.07 ev). This spectrum was originally analyzed in 198 by H. A. Robinson to find the energy levels. These studies have being used in the compilation of Atomic Energy Levels published by C. E. Moore [1], although a wavelength list has never been published. R. L. Kelly in Ref. [] has included some of these lines as given by Moore in his first compilation. Later in 1970, Fawcett [3], using a theta-pinch as light source, identified wavelengths of transitions occurring in the interval - 1 Å and Å. Fawcett et al. [] using laser-produced plasma experiments confirmed the identity of many of their previous obtained lines classification. Goldsmith et al. added, revised and extended the analyses performed by Robinson and Fawcett, classifying 13 lines in the range 3-39 Å with the transitions s-np, p-3s, and p-nd. Kasyanov et al. [6] and Dere [7] realized measurements of the transition 1s p P 3/ to the How to cite this paper: Mania, A.J. and Luna, F.R.T. (016) Oscillator Strengths and Lifetimes for the P XIII Spectrum. Spectral Analysis Reviews,,

2 ground level 1s s S 1/. Deschepper et al. [8] using a Doppler-tuned X-ray absorption technique realized measurements to the transition 1s s S 1/ -1ssp P 1/ and P 3/. Edlén [9], using series formulae, has given results for the 1s nl systems that are in agreement with the expected experimental errors. Wavelengths observed by Fawcett and Ridgeley [10] and Goldsmith et al. in the region Å, were used in the spectral analysis to evaluate the p and f levels, being that the s levels were evaluated from isoelectronic sequence values for p - s separations. Aglitskii et al. and Boiko et al. [1], using laser-produced plasma, have contributed to the spectral features that have been observed in transitions of doublet term of the configurations 1ss, 1sp, 1ssp, 1ss3p, 1ssp, 1sp3p, 1spp, where the levels were derived from energy separations calculated by Vainshtein and Safronova [13] [1]. The wavelength tables given by these publications [15] [16], are lines arranged by spectra, being some lines of P XIII spectra which are not in other references. Martin et al. [17] compiles all the energy levels of all the phosphorus ions, revising the earlier version of Moore of all the published data so far, as well as the unpublished data of Robinson. Hayes and Fawcett [18] give a new original contribution by using the same spectrum obtained in theta-pinch experiment earlier. Kelly [19] reviews all P XIII line identifications in his compilation. Recently, Wang et al. [0]-[] has published data of oscillator strengths for 1s s to 1s np, and 1s p to 1s nd transitions of the Lithium isoelectronic sequence.. Methodology Computations of wavelengths made with the aid of a Hartree-Fock Relativistic (HFR) computer program package and a program of least-square procedure as given by Cowan [3] to adjust the values of the energetic parameters, comparing the data and calculating its consistency with the identification of known energy levels. The adjustable parameters are to be determined empirically to give the best possible fitting between the calculated eigenvalues and the observed energy levels. The fitting process is carried out by a self-consistent procedure until the parameter values no longer change from one iteration cycle to the next. The main purpose is to reach a fitting to the experimental energy levels, which minimizes the uncertainties as much as possible, using the least-squares method for each parity in which the standard deviation is less than one percent of the energy range covered by the energy levels. The optimized electrostatic parameters substitute their corresponding theoretical values and they are used again to calculate energy matrices, the determination of the oscillator strengths and lifetimes values. All strong configuration interactions are to be included and HFR method is used to given a better accuracy []. It should also be noticed, that at higher levels, the j-j notation is better and it should be used to estimate the percentages of compositions. The oscillator strengths f ( γ, γ ) is a physical quantity related to line intensity I and transition probability W γ, γ, by: ( ) ω e W ( γ, γ ) = f 3 ( γ, γ ), (1) mc With I gw ( γ, γ ) g f ( γ, γ ) = gf, being m the electron mass, e their charge, γ the initial quantum state, ω = ( E( γ) E( γ )) ħ, E(γ) the initial state energy and g = (J + 1) is the number of degenerate quantum states with angular momentum J. Quantities with primes refer to the final state. In the equation above, the weighted oscillator strength, gf, is 8π mca0σ gf = S, () 3h where σ = E ( γ) E ( γ ) hc, h is Planck s constant; c is the light velocity; and a 0 is the Bohr radius. The electric dipole line strength is defined by: 1 γj γ J S = P (3) This quantity is a measure of the total strength of the spectral line, including all possible transitions between mm and J z eigenstates. The tensor operator P 1 (first order) in the reduced matrix element is the classical dipole moment for the atom in units of ea 0. To obtain gf, we need to calculate S first, or its square root 1 1 S = S = J P J. () γγ γγ γ γ

3 In a multiconfiguration calculation we have to expand the wavefunction wavefunction, β J, for both upper and lower levels: γ J in terms of single configuration γj = y βj (5) γ β β J Therefore, we can have the multiconfigurational expression for 1 S γγ 1 γ 1 γ S γγ yβ J βj P β J y β β β J (6) = The probability per unit time of an atom in a specific state γj to make a spontaneous transition to any state with lower energy is P( γj) = A( γj, γ J ) (7) where A( γj, γ J ) is the Einstein spontaneous emission transition probability rate for a transition from the γ J to the γ J state. The sum is over all γ J states with E( γ J ) < E( γj). The Einstein probability rate is related to gf through the following relation by: Since the natural lifetime τ ( γj) A( γj, γ J ) 8π e σ ga = gf (8) mc ( ) 1 =. The natural lifetime is applicable to an isolated atom. The interaction with matter or radiation will reduce the lifetime of a state. The values for gf and lifetime given in Table 1 and Table, respectively, were calculated according to these equations. In order to obtain better values for oscillator strengths, we calculated the reduced matrix elements P 1 by using optimized values of energy parameters which were adjusted from a least-squares calculation. In this adjustment, the code tries to fit experimental energy values by varying the electrostatic parameters. This procedure improves σ values used in Equation () and y γ and β J y γ β J values used in Equation (6). Wavelength values in vacuum were converted to air by the relation, λvac = nλair, where the index of refraction of standard air (dry air containing 0.03CO by volume at normal pressure and T = 15 C ) is 3. Results and Discussion n σ σ 8 = In our fitting process, the standard deviation reached for each parity as 1 cm 1 and 5 cm 1, for even and odd configurations, respectively, is satisfactory for the aims of this work. Values for gf and lifetime given in Table 1 and Table, respectively, were calculated by the previously described method. Table 1 shows the results of the comparison between wavelength values as calculated by the method and the observed. In Table, we present lifetimes, energy levels and an estimation of their percentage composition. For the even-parity configurations we have the following picture: 1s 5g, 1s 6g, 1s 6s, 1s 7s, 1s 8s, 1s 7d, 1s 8d, 1ss, and the series 1spnp (3 n ). For the odd-parity case we study the configuration 1s 6h, and the series 1s nf ( n 6), 1s np (5 n 8), 1ssnp ( n ). The interpretation of the configuration levels structure was made by least-squares fit of the observed levels and we propose the new values possible of the energy levels marked with asterisk (*) in the table. The oscillator strengths and lifetimes for the lithium-like ions are of astrophysical interest for photo-ionization modelling of elemental abundances in cosmic objects since an extensive data source is not currently available. Transitions in this ion have been of particular importance in extrapolation analysis especially for the dense spectra from N-like sequence in which the phosphorus is one element in isoelectronic sequence linking lighter elements where the analysis is more extensive. Is also an important testing ground for the development of theoretical methods which attempt to calculate atomic structure of many-electron systems.. Conclusion We have presented oscillator strengths and lifetimes for all known transitions in P XIII. The gf-values are better agreement with line intensity observations and lifetime values that are closer to the experimental ones. We have been stimulated by the need to determine both important parameters in the study of plasma laboratory and solar 3

4 Table 1. Oscillator strengths and spectral lines for P XIII in the vacuum. gf-value Int. Lambda (Å) Levels (cm 1 ) Configurations Terms Ref. Obs. Calc. Even-Odd ,886,130 1s s - 1s( 1 S)sp( 3 P) ,886,60 1s s - 1s( 1 S)sp( 3 P) ,07,30-08,0 1s( 1 S)pp( 1 P) - 1s p ,07,30-19,30 1s( 1 S)pp( 1 P) - 1s p S1/ - P 3/ S1/ - P 1/ P1/ - P 1/ P1/ - P 3/ ,018,60-08,0 1s( 1 S)pp( 3 P) - 1s p ( 1 P) D 3/ - P 1/ ,019,0-19,30 1s( 1 S)pp( 3 P) - 1s p ( 1 P) D 5/ - P 3/ ,99,895 1s ( 1 S)s - 1s( 1 S)s3p( 3 P) ,951,015 1s ( 1 S)s - 1s( 1 S)s3p( 3 P) S1/ - P 3/ S1/ - P 1/ ,91,85 1s s - 1s( 1 S)s3p( 1 P) ( 3 P) S 1/ - P 3/ ,90,70 1s s - 1s( 1 S)s3p( 1 P) ( 3 P) S 1/ - P 1/ ,00,65-08,0 1s( 1 S)p3p( 1 P) - 1s p ( 1 P) S 1/ - P 1/ ,00,65-19,30 1s( 1 S)p3p( 1 P) - 1s p ( 1 P) S 1/ - P 3/ ,09,775-19,30 1s( 1 S)p3p( 1 P) - 1s p ( 1 P) D 5/ - P 3/ [19] ,98,570-08,0 1sp - 1s p ,98,570-19,30 1sp - 1s p ,6,350 1s s - 1s( 1 S)sp( 1 P) ,61,115 1s s - 1s( 1 S)sp( 1 P) ,191,815 1s s - 1s( 1 S)sp( 3 P) ,186,895 1s s - 1s( 1 S)sp( 3 P) S1/ - P 1/ S1/ - P 3/ S1/ - P 3/ S1/ - P 1/ S1/ - P 3/ S1/ - P 1/ ,00,65-08,0 1s( 1 S)p3p( 1 P) - 1s p ( 1 P) S 1/ - P 1/ ,378,605-08,0 1sp - 1s p ,388,180-19,30 1sp - 1s p * ,00,00-0,886,60 1s s - 1ssp P1/ - P 1/ P3/ - P 3/ S1/ - P 1/ * ,00,00-0,886,130 1s s - 1ssp S1/ - P 3/ * ,90,65-37,7,00 1spp - 1s f D5/ - F 5/ * ,90,65-37,73,800 1spp - 1s f D5/ - F 7/ ,353,875-08,0 1sp - 1s p ,353,875-19,30 1sp - 1s p ,355,065-19,30 1sp - 1s p D3/ - P 1/ D3/ - P 3/ D5/ - P 3/ * ,788,650-19,91,85 1s3s - 1ss3p * ,788,650-19,90,70 1s3s - 1ss3p S1/ - P 1/ S1/ - P 3/ ,51,90-08,0 1sp - 1s p ,6,905-08,0 1sp - 1s p ,57,990-19,30 1sp - 1s p ,51,90-19,30 1sp - 1s p ,6,905-19,30 1sp - 1s p P3/ - P 1/ P1/ - P 1/ P5/ - P 3/ P3/ - P 3/ P1/ - P 3/ * ,08,110 1ss - 1ssp S1/ - P 3/

5 Continued * ,0,00 1ss - 1ssp S1/ - P 1/ / ,633,565-19,30 1s 8d - 1s p /.678 *.659,633,86-19,30 1s 8d - 1s p / ,553,085-19,30 1s 7d - 1s p D5/ - P 3/ [] D3/ - P 3/ [] D5/ - P 3/ [] /.075 * 3.076,55,860-19,30 1s 7d - 1s p D3/ - P 3/ [] ,19,350-08,0 1s 6d - 1s p ,19,350-19,30 1s 6d - 1s p ,19,350-19,30 1s 6d - 1s p ,19,300-08,0 1s 5d - 1s p ,19,300-19,30 1s 5d - 1s p ,193,00-19,30 1s 5d - 1s p D3/ - P 1/ D5/ - P 3/ D3/ - P 3/ D3/ - P 1/ D5/ - P 3/ D3/ - P 3/ * ,181,300-08,0 1s 5s - 1s p S1/ - P 1/ ,758,169 1s s - 1s p ,758,11 1s s - 1s p ,773,500-08,0 1s d - 1s p ,77,000-19,30 1s d - 1s p S1/ - P 3/ S1/ - P 1/ D3/ - P 1/ D5/ - P 3/ * ,773,500-19,30 1s d - 1s p * ,70,00-08,0 1s s - 1s p * 8.0 3,70,00-19,30 1s s - 1s p D3/ - P 3/ [16] [17] S1/ - P 1/ S1/ - P 3/ ,89,10 1s s - 1s 3p ,86,080 1s s - 1s 3p ,870,50-08,0 1s 3d - 1s p ,871,530-19,30 1s 3d - 1s p ,870,50-19,30 1s 3d - 1s p ,788,650-08,0 1s 3s - 1s p ,788,650-19,30 1s 3s - 1s p ,19,300 -,86,080 1s 5d - 1s 3p S1/ - P 3/ S1/ - P 1/ D3/ - P 1/ D5/ - P 3/ D3/ - P 3/ S1/ - P 1/ S1/ - P 3/ D3/ - P 1/ * 7.66,19,300 -,89,10 1s 5d - 1s 3p D3/ - P 3/ ,19,300 -,89,10 1s 5d - 1s 3p / ,30 1s s - 1s p / ,0 1s s - 1s p ,788,650 -,89,10 1s 3s - 1s 3p ,788,650 -,86,080 1s 3s - 1s 3p ,70,00-3,76,550 1s s - 1s p ,871,530 -,89,10 1s 3d - 1s 3p ,870,50 -,89,10 1s 3d - 1s 3p D5/ - 3/ S1/ - P5 / [6]-[8] S1/ - P 1/ [6]-[8] S1/ - P 3/ [15] [16] S1/ - P 1/ [15] [16] S1/ - P 3/ [15] [16] D5/ - P 3/ [15] [16] D3/ - P 3/ [15] [16] 5

6 Table. (a) Even configurations. (b) Odd configurations. Lifetimes (s) Energy levels (cm 1 ) Configurations Terms Percentage Composition (a) 0 1s s ,788,650 1s 3s ,870,50 1s 3d ,871,530 1s 3d ,70,00 1s s ,773,500 1s d ,77,000 1s d ,181,300 1s 5s ,19,300 1s 5d ,19,300 1s 5d *,199,70 1s 5g *,199,330 1s 5g *,15,60 1s 6s ,19,350 1s 6d ,19,350 1s 6d *,5,975 1s 6g *,6,010 1s 6g *,556,00 1s 7s *,55,860 1s 7d ,553,085 1s 7d *,67,077 1s 8s *,633,5 1s 8d ,633,565 1s 8d S1/ 100% S1/ 100% D3/ 100% D5/ 100% S1/ 100% D3/ 100% D5/ 100% S1/ 100% D3/ 100% D5/ 100% G5/ 100% G7/ 100% S1/ 100% D3/ 100% D5/ 100% G5/ 100% G7/ 100% S1/ 100% D3/ 100% D5/ 100% S1/ 100% D5/ 100% D5/ 100% * 16,971,300 1ss ( S) S1/ 9% + 8% 1sp ( 1 S) S ,6,905 1sp ( 3 P) P1/ 100% ,51,90 1sp ( 3 P) P3/ 100% ,57,990 1sp ( 3 P) P5/ 100% ,353,875 1sp ( 1 D) D3/ 97% ,355,065 1sp ( 1 D) D5/ 100% ,378,605 1sp ( 3 P) P1/ 100% ,388,180 1sp ( 3 P) P3/ 97% ,98,570 1sp ( 1 S) S1/ 91% + 8% 1ss ( S) 6

7 Continued * 19,97,700 1sp3p ( 3 P) D1/ 95% * 19,797,615 1sp3p ( 3 P) D3/ 96% * 19,80,55 1sp3p ( 3 P) D5/ 99% * 10,809,080 1sp3p ( 3 P) D7/ 100% * 19,816,705 1sp3p ( 3 P) S3/ 56% + 39% 1sp3p( 3 P) P * 19,867,315 1sp3p ( 3 P) P3/ 50% + 1% 1sp3p( 3 P) S * 19,867,0 1sp3p ( 3 P) P1/ 89% + 5% 1sp3p ( 3 P) D + 5% 1sp3p( 1 P) P * 0,01,950 1sp3p ( 1 P) D3/ 89% + 9% 1sp3p( 3 P) D ,09,775 1sp3p ( 1 P) D5/ 9% + 6% 1sp3p( 3 P) D ,00,65 1sp3p ( 1 P) S1/ 79% + 19% 1sp3p( 3 P) S * 0,3,915 1sp3p ( 3 P) P1/ 99% * 0,35,950 1sp3p ( 3 P) P3/ 96% * 0,330,500 1sp3p ( 3 P) P5/ 99% * 0,3,0 1sp3p ( 3 P) D3/ 89% + 9% 1sp3p( 1 P) D * 0,35,930 1sp3p ( 3 P) D5/ 93% + 6% 1sp3p( 1 P) D * 0,68,175 1sp3p ( 3 P) S1/ 80% + 18% 1sp3p( 1 P) S * 0,559,010 1sp3p ( 1 P) P1/ 91% + 6% 1sp3p( 3 P) P * 0,56,875 1sp3p ( 1 P) P3/ 91% + 7% 1sp3p( 3 P) P * 0,913,970 1spp ( 3 P) D1/ 9% + 7% 1spp( 3 P) P * 0,916,30 1spp ( 3 P) D3/ 9% ,90,65 1spp ( 3 P) D5/ 93% + 6% 1spp( 3 P) P * 0,97,5 1spp ( 3 P) D7/ 100% * 0,9,595 1spp ( 3 P) S3/ 9% + 5% 1spp( 3 P) P + % 1spp( 3 P) P * 0,95,580 1spp ( 3 P) P1/ 7% + 0% 1spp( 3 P) P * 0,97,915 1spp ( 3 P) P1/ 77% + 16% 1spp( 3 P) P * 0,930,500 1spp ( 3 P) P3/ 60% + 19% 1spp( 3 P) S + 1% 1spp( 3 P) D * 0,933,730 1spp ( 3 P) P3/ 67% + 31% 1spp( 3 P) S * 0,93,970 1spp ( 3 P) P5/ 9% + 6% 1spp( 3 P) D * 0,939,950 1spp ( 3 P) D3/ 85% + 1% 1spp( 3 P) P * 0,96,885 1spp ( 3 P) D5/ 97% * 0,956,590 1spp ( 3 P) S1/ 9% ,018,60 1spp ( 1 P) D3/ 97% ,019,0 1spp ( 1 P) D5/ 100% * 1,00,865 1spp (1 P) P1/ 97% * 1,0,50 1spp ( 1 P) P3/ 97% ,07,30 1spp ( 1 P) S1/ 97% ( * ) Indicates an attempt to identify. 7

8 (b) Lifetimes (s) Energy levels (cm 1 ) Configurations Terms Leading Percentage ,0 1s p ,30 1s p ,86,080 1s 3p ,89,10 1s 3p ,756,701 1s p ,76,58 1s p * 3,77,0 1s f * 3,77,380 1s f *,193,330 1s 5p *,193,980 1s 5p *,199,015 1s 5f *,199,115 1s 5f *,,58 1s 6p *,,90 1s 6p *,5,85 1s 6f *,5,885 1s 6f *,6,05 1s 6h *,6,050 1s 6h *,560,55 1s 7p *,560,760 1s 7p *,69,965 1s 8p *,650,10 1s 8p P1/ 100% P3/ 100% P1/ 100% P3/ 100% P1/ 100% P3/ 100% F5/ 100% F7/ 100% P1/ 100% P3/ 100% F5/ 100% F7/ 100% P1/ 100% P3/ 100% F5/ 100% F7/ 100% H9/ 100% H11/ 100% P1/ 100% P3/ 100% P1/ 100% P3/ 100% ,0,00 1ssp ( 3 S) P1/ 100% ,08,110 1ssp ( 3 S) P3/ 100% * 17,035,000 1ssp ( 3 S) P5/ 100% ,186,895 1ssp ( 1 P) P1/ 61% + 39% 1ssp( 3 S) P ,191,815 1ssp ( 3 S) P3/ 50% + 50% 1ssp( 1 S) P ,61,115 1ssp ( 3 S) P1/ 61% + 39% 1ssp( 1 S) P ,6,350 1ssp ( 1 P) P3/ 50% + 50% 1ssp( 3 S) P ,90,70 1ss3p ( 3 S) P1/ 100% ,91,85 1ss3p ( 3 S) P3/ 100% * 19,93,960 1ss3p ( 3 S) P5/ 100% ,99,895 1ss3p ( 3 S) P3/ 99% ,951,015 1ss3p ( 3 S) P1/ 100% * 0,05,080 1ss3p ( 1 P) P1/ 100% 8

9 Continued * 0,057,670 1ss3p ( 1 P) P3/ 100% * 0,851,70 1ssp ( 3 S) P1/ 100% * 0,851,760 1ssp ( 3 S) P3/ 100% * 0,85,600 1ssp ( 3 S) P5/ 100% ,886,130 1ssp ( 3 S) P3/ 99% ,886,60 1ssp ( 3 S) P1/ 99% * 0,987,90 1ssp ( 1 P) P1/ 99% * 0,989,30 1ssp ( 1 P) P3/ 99% ( * ) Indicates an attempt to identify. spectra, as also phosphorus is an astrophysically important element. The present work is part of an ongoing program, whose goal is to obtain weighted oscillator strength, gf, and lifetimes for elements of astrophysical importance. Phosphorus occupies the fifteenth place with respect to cosmic distribution [6]. References [1] Moore, C.E. (199) Atomic Energy Levels. Vol. 1, Circular of the National Bureau of Standards, Washington DC. [] Kelly, R.L. and Palumbo, L.J. (1973) Atomic and Ionic Emission Lines below 000 Angstroms: Hydrogen through Krypton. NRL Report 7599, Tune. [3] Fawcett, B.C. (1970) Classification of Highly Ionized Emission Lines due to Transitions from Singly and Doubly Excited Levels in Sodium, Magnesium, Alumninum, Silicon, Phosphorus, Sulphur, and Chlorine. Journal of Physics B, 3, [] Fawcett, B.C., Hardcastle, R.A. and Tondello, G. (1970) New Classifications of Emission Lines of Highly Ionized Phosphorus and Sulphur. Journal of Physics B, 3, Goldsmith, S., Oren, L. and Cohen, L. (1973) Spectra of P XII and P XIII in the Extreme Vacuum Ultraviolet. Journal of the Optical Society of America, 63, [6] Kasyanov, Y.S., Konomov, E.Y.A., Korobkin, V.V., Koshelev, K.N. and Serov, R.V. (1973) Intrashell Transitions in the Spectra Multicharged Phosphorus Ions. Optics and Spectroscopy (URSS), 35, [7] Dere, K.P. (1978) Spectral Lines Observed in Solar Flares between 171 and 630 Angstroms. Astrophysics, 1, [8] Deschepper, P., Lebrunm, P., Palffy, L. and Pellegrin, P. (198) Energy and Lifetime Measurements in Heliumlike and Lithiumlike Phosphorus. Physical Review A, 6, [9] Edlen, B. (1983) Comparison of Theoretical and Experimental Level Values if the n = Complex in Ions Isoelectronic with Li, Be, O and F. Physica Scripta, 8, [10] Fawcett, B.C. and Ridgeley, A. (1981) Analysis of n = 3 to n = Spectra for Ions from Mg X to Fe XXIV and P XI, XII. Journal of Physics B: Atomic and Molecular Physics, 1, Aglitskii, E.V., Boiko, V.A., Zakharov, S.M., Pikuz, S.A. and Faenov, A.Y.A. (197) Observation in Laser Plasmas and Identification of Dielectron Satellites of Spectral Lines of Hydrogen- and Helium-Like Ions of Elements in the Na- V Range. Soviet Journal of Quantum Electronics,, [1] Boiko, V.A., Faenov, A.Y. and Pikuz, S.A. (1978) X-Ray Spectroscopy of Multiply-Charged Ions from Laser Plasmas. Journal of Quantitative Spectroscopy & Radiative Transfer, 19, [13] Vainshtein, L.A. and Safronova, U. (1975) Wavelengths and Transition Probabilities for Ions. I ISAN Report, Troitsk, Russia, N6, [1] Vainshtein, L.A. and Safronova, U. (1978) Wavelengths and Transition Probabilities of Satellites to Resonance Lines of H- and He-Like Ions. Atomic Data and Nuclear Data Tables, 1, [15] (1980) Wavelengths and Transition Probabilities for Atoms and Atomic Ions Part 1: Wavelengths; Part : Transition Probabilities. NSRDS-NBS, Washington DC, 68. 9

10 [16] Reader, J. and Corlis, C.H. (198) Line Spectra of the Elements. In: Weast, R.C., Ed., CRC Handbook of Chemistry and Physics, 63rd Edition, CRC Press, Boca Raton. [17] Martin, W.C., Zalubas, R. and Musgrove, A. (1985) Energy Levels of Phosphorus, P I through P XV. Journal of Physical and Chemical Reference Data, 1, [18] Hayes, R.W. and Fawcett, B.C. (1986) The Spectrum of Phosphorus VI to XIII Between and 9 Å. Physica Scripta, 3, [19] Kelly, R.L. (1987) Atomic and Ionic Spectrum Lines below 000 Angstroms: Hydrogen through Krypton. Journal of Physical and Chemical Reference Data, 16, [0] Hu, M.-H. and Wang, Z.-W. (00) Oscillator Strengths for P - n D Transitions of Lithium-Like Systems with Z = 11 to 0. Chinese Physics, 13, [1] Chen, C. and Wang, Z.-W. (005) Oscillator Strengths for s - p P Transitions of the Lithium Isoelectronic Sequence from NaIX to CaXVIII. Communications in Theoretical Physics, 3, [] Hu, M.-H. and Wang, Z.-W. (009) Oscillator Strengths for S - n P Transitions of the Lithium Isoelectronic Sequence from Z = 11 to 0. Chinese Physics B, 18, [3] Cowan, R.D. (1981) The Theory of Atomic Structure and Spectra. University of California Press, Berkeley. [] Owens, J.C. (1967) Optical Refractive Index of Air: Dependence on Pressure, Temperature and Composition. Applied Optics, 6, Fawcett, B.C. (1991) On the Accuracy of Oscillator Strengths. In: Wilson, S., Grant, I.P. and Gyorffy, B.L., Eds., The Effects of Relativity in Atoms, Molecules, and the Solid State, Springer, New York, 5-5. [6] Aller, L.H. (1963) Distribution of the Chemical Elements. Foreign Literature Press, Moscow. 10

Energy Levels, Oscillator Strengths, and Transition Probabilities of Ni XIX and Cu XX

Optics and Photonics Journal, 2014, 4, 54-89 Published Online March 2014 in SciRes. http://www.scirp.org/journal/opj http://dx.doi.org/10.4236/opj.2014.43008 Energy Levels, Oscillator Strengths, and Transition