Transition Probabilities for the Dipole Allowed Fine Structure Transitions in S II

Transcription

1 Physica Scripta. Vol. 55,00-3, 1997 Transition Probabilities for the Dipole Allowed Fine Structure Transitions in S II Sultana N. Nahar Department of Astronomy, The Ohio State University, Columbus, Ohio, U.S.A. 3 Received December 1,1995; accepted in revisedform March,199 Abstract The atomic quantities for bound-bound transitions such as the oscillator strengths, the line strengths, and the Einstein A-coefficients are obtained for a large number of dipole allowed (AS = 0) transitions for the astrophysically important ion SII. The oscillator strengths in LS coupling are obtained in an ab initio manner in the close coupling approximation using R-matrix method. The quantities for the fine structure transitions are obtained through an algebraic transformation of the LS values. The spectroscopic energies of the fine structure levels are used instead of the calculated energies to improve the accuracy of these values. Present calculations employs a 17-state eigenfunction expansion of the SI11 core states. Results are presented for 1 h e structure dipole allowed transitions in S I1 corresponding to 350 transitions in LS coupling. This work reports the rst extensive tabulation of S I1 radiative transitions including fine structure. Comparison is made with the available experimental and theoretical data and good agreement is found with the observed values and other accurate theoretical works. 1. Introduction SI1 is an astrophysically important ion [l], but like most other comparatively larger ions, theoretical studies for the radiative transition probabilities of this ion were carried out only in a small limited scale. However, accurate as well as extensive data are needed for the interpretation of observations being made, such as sulfur emission spectra of the plasma torus of Jupiter s satellite Io by Voyager I and I1 []. Furthermore, collisional rate coefficients have recently been computed for a large number of transitions in SI1 [3] and it is desirable to complement the atomic datasets for astrophysical modeling with radiative data. The first extensive work on S I1 was carried out by Butler et al. [] under the Opacity Project (OP) [5]. Like all OP calculations, their work was also carried out in LS coupling. But for laboratory plasma experiments and for a variety of astrophysical model applications, it is often the fine structure transitions that are required, rather than the LS values. The purpose of the present work is to provide a reasonably complete set of oscillator strengths ($values), line strengths (S-values) and the transition rates (A-values) for the dipole allowed fine structure transitions in SII. The method has been applied to several other ions [, 71, and is briefly summerized below.. Summary of the theoretical work and computations The calculations for the atomic parameters of the fine structure transitions are based on obtaining the line strength, S, in an ab initio manner in the close coupling (CC) approximation. In the CC approximation the core ion, termed as the target, is represented by an N electron system. The wavefunction expansion, Y(E), for any symmetry, SLx, of the total (N + 1) electron system is represented in terms of the target states as : i j where xi is the target ion wave function in a speci ic state Si Li xi and Oi is the wave function for the (N + 1)th electron in a channel labeled as SiLi xi k: li(slx); k? being its incident kinetic are the correlation wavefunctions of the (N + 1) electron system that compensates the orthogonality condition of the total wavefunction. The CC sums imply extensive configuration interactions in the coupled wavefunctions for each SLx. Therefore, provided the relativistic effects are small, the ab initio computations for the derived transition matrix elements should be accurate. The line strength, S, for transition between the initial i and the final f states is obtained as S I<yfIIDIIYi)I, () where the operator D is It in length form, the sum going over total number of electrons in the ion, and Yi, Yf are the initial and final wavefunc- tions respectively. The line strength depend on the wavefunctions, not on the energies, of these states. As we expect the present CC wavefunctions to be very accurate, it is possible to obtain improved oscillator strengths by using observed, rather than calculated, energy differences. Using the energy difference, Efi, of the initial and final states, the oscillator strength, fif, for the transition can be obtained from S as and the Einstein s A-coefficient, AJi, as where tl is the fine structure constant, and gi, gf are the statistical weight factors of the initial and final states, respectively. In terms of c.g.s. unit of time, Afi(a.u.) Afi(K1) = 9 70 where zo =.191- s is the atomic unit of time. For the present work, the values of Efi are used from the observed energies. (3) () (5)

2 Transition Probabilities for the Dipole Allowed Fine Structure Transitions in S II 01 Table I. The 17 states of S III employed in the close coupling eigenfunction expansion of S II 3s3pz 3s3pz 3s3p3 3s3p3 3s3p3 3s3p3d 3s3p3d 3s3p3d 3s3p3d 3p= 'S' 3Do ' Do ' Po P" 3Do 'D" 'PO 3s3p 3s3p3 3s3p3 3s3p3d 3s3p3 3s3ps 3s3ps 3s3p3d 'D' so 3P" 3F0 3 so 3P0 'PO ' F" Spectroscopic configurations: 3s3p, 3s3p3, 3s3p3d, 3s3ps Correlation congurations: 3s3p3d, 3s3dZ, 3p, 3p33d, 3s3p3dZ, 3p3s The fine structure line strengths, SJJ, are obtained from the LS multiplet strength, SLs, through the algebraic transformation as Sjj = C,r(Ji, Jf)S,s/[(Si + 1)(Li + 1)(L, + I)], (7) for the allowed transitions (AJ = 0, k 1). Si is the spin multiplicity which remains the same (Si = S,) during the transitions. The values of the coefficients CAl(J,, J,) are obtained from Allen []. The SJJ values satisfy the condition The fine structure f-values, fjj, can also be obtained directly from the LS oscillator strengths, fls, as [9] fjj(nf Si L, J,, ni Si Li Ji) = fls(ns Si L,, ni Si Li)(J, + 1) x (Li + l)wz(l,lij,ji; lsj, where W(L, Li J, Ji; lsi) is a Racah coefficient. The above values also satisfy sum 1 (51 + l)fjj(nf JiJf Si L, J, 3 ni Si Li Ji) (9) = (Si + 1)(Li + l)fls(nf S,L,, ni Si Li). () Both algebraic transformations yield fine structure components with about the same accuracy. In the first case the fine structure splitting is carried out for the LS line strengths whereas in the latter case for the LSfvalues. The first transformation is more convenient to use when observed levels are available. The direct transformation of fvalues is used Table 11. Absolute measured (expt) and calculated (calc) energies (in Rydberg unit) of S II. The negative sign of the energies are not shown. The degeneracy of the states are assinged in ascending order for the even parity and descending order for the odd parity states belonging to the same symmetry. An ast erisk next to a state indicates incomplete set of observed energy levels for the state. Term E (expt) E (calc) Term E (expt) E (calc) s" z Po a 'Dm b Pe b 'Pe a 'Fe b 'D' a 'G' z P" y 'Do y ' PO b 'SC c 'PC x 'Do d 'De e ZD' e Pc b Fc e Pc w zpo y P" W 'D" f 'De b 'G' f P' h 'Po c Dc gpc d 'Se i 'Pc h Pr d "D; i Pn c 'GC j Pc s3p3 3s3p 3~'3p'(~P)3d 3~'3p~(~P)3d 3~'3p'(~P)3d 3s3p 3s'3p'(3P)p 3s3p'(3P)p 3~'3p'(~P)3d 3s'3p'(("P)p 3s3p('P)3d 3s3pZ('D)3d 3s3p('D)p 3s3pZ('D)p 3s3p 3s'3p(3P)5s 3s'3p('D)3d 3~'3p'(~P)d 3~'3p'(~P)d 3s3p'('P)5p 3s3p'(3P)5p 3~'3p'(~P)d 3s3p'('D)5s 3s3p('D)d 3s3p'('D)d 3~'3p'(~P)Sd 3s3p( ' D)d 3s'3pZ('D)5p 3~'3p'(~P)Sd 3~'3p~(~P)Sd 3s3p(3P)7s 3~'3p'(~P)d 3s3p( 'D)s 3~'3p'(~P)7d 3s3~'('D)7s -. I Z'D" a Pe a 'Po a Fs a Dc a 'Se z 'so z Do c P' y s0 c 'De b 'Fe Z 'F" x 'PO d 'P' d Pe c 'se b Dc c 'Fe y D0 x so f 'PO g 'De d 'Fe g P' c Fs h 'De y 'FO e 'Fe i 'De j 'Pc d F: j 'De e D' k 'De

3 0 S. A. Nahar for the LS multiplets where a complete set of observed fine structure levels is unavailable for one or both the terms, and for transitions between high angular momentum states (transitions higher than H tt I). Calculated energies are used for these cases. The lifetime of a state can be obtained easily once the A-values of the state are known as 1 ~ 7, = -, A, where A, is the total radiative transition probability for the statej; i.e., A, = c AYi (1) i The present work on LS oscillator strengths for SI1 is carried out in a similar manner to the OP work [], but employing a 17-state eigenfunction expansion which inclues the s orbital (the OP expansion with 15-states does not include the s orbital); the relevant data for SI11 are given in Table I. The 17 states, dominated by configurations 3s3p, 3s3p3, 3s3p3d, and 3s3ps, of the core ion S 111, are optimized using the atomic structure code SUPER- STRUCTURE [lo]. The theoretical details of the close coupling approximation using the R-matrix method are described in Ref. [5]. The computations are carried out using the R-matrix codes [11] as developed for the OP [5]. The number of radiative transitions in S I1 in the present work exceeds that of the previous OP calculations [], and includes 31 LS bound states below the first ionization threshold and 500 LS multiplets. A comparison is made of the present calculated energies with the observed ones in Table 11. The observed LS energies are obtained through statistical average of the observed fine structure level energies. An asterisk next to a state in the table indicates incomplete set of observed energy levels for the state. The number of observed bound states of S I1 is smaller, 70 LS terms in total [1], than the number of calculated bound states, 31. The calculated energies are within 5% difference of the 5 observed LS energies; the other 5 are within %. For the fine structure transitions the algebraic transformations of the LS values are carried out as described above, with improved accuracy using spectroscopically observed energies, and employing the computer code JJTOLS [7]. Results are obtained for transitions between only those LS states that have been observed, with either complete or incomplete set of observed fine structure levels. Each observed LS term has been designated by a degeneracy symbol, as shown in Table 11, and is employed in representing the transitions in this work. This degeneracy assignment may not necessarily match the observed one; an ascending order of alphabets is chosen for the observed even parity states of a symmetry, while a descending order is chosen for the observed odd parity states. In order to ascertain the accuracy of the present results, comparison is made with available theoretical and experimental values on SI1 in Table 111. Present f-value for the transition 3s3p3(z 'Do)-+ 3s3ps(bDe) agrees very well with the $value obtained from the beam-foil experiment by Ryan et al. [ 11 in comparison to other calculations such as by Butler et al. [] and Ojha and Hibbert [13]. Among the available theoretical calculations, the works of Butler et al. [] and Ojha and Hibbert [13] are the most elaborate ones, the former using the R-matrix close coupling method and the latter from an optimised configuration-interaction type atomic structure calculation. For the other transition 3s3p3(z P0) --f 3s3ps@ 'De) the present f-value is signscantly lower than that by Ryan et al. [1]. This experimental f-value is much higher than the calculated value by Butler et al. [] as well indicating a possible overestimation in the measured value. Thef-value of both Butler et al. [] and Ojha and Hibbert [13] agree very well with the measured value of Lawrence [15] in pulsed-beam experiment for the transition z S0 -+ a Pe, whereas the present f-value is about 1% higher. This difference is reflected in the lifetime comparison as well, presented in the lower part of the table, for the fine structure components 3s3p(a Pe)5/, 3/, of the same multiplet obtained from the same measurement by Lawrence [15]. The calculated f-value by Cai and Pradhan [3] is lower than the measured value; their calculations were primarily intended for collisional data for S I1 and not particularly optimized for radiative quantities. The present $values are compared for a few more transitions with the other calculations, and all theoretical values are found to be in reasonable agreement with each other for the strong transitions. However, Ojha and Hibbert [13] obtain a higher value for the transition z S0 -+ b Pe compared to the other calculations. For the relatively weak transition z 'Po + a 'Se the present f-value agrees with Ojha and Hibbert, while for z 'Po --f a 'De they agree better with Table 111. Comparison of the present $values and lifetimes (7). fir Transition Present Expt. The0 z'd" + a 'De 'D" + b 'De z'd" + c 'De zp" + a 'se z'p" + a 'D' z'p" + b 'De Z'P" -9 C'D' zs0 -, ap' zs0 -, by s" -, C~P' b, O.OllC, 0.01' 0.1 (0.0)g 0.15b, 0.151' 0.1b, 0.15', 0.1' 0.00", 0.00' O.OO1lb, c, 0.001' 0.0 (0.1). 0.01b 0.3b, 0.33' 0.03 (0.00)d 0.03b, 0.039", 0.0' 0.3b, 0.0', 0.33'.3b.."..' 7 (ns) State Present Expt. Theo. 3. Results and discussion ap' ()d apc ()d ape 1/ ()d The$, S, and A-values are obtained for a large number of fine structure transitions in SII. These results Drovide the first extensive set of fine structure transitions in S 11. The earlier calculations are mainly for LS transitions and are limited to a small number of transitions except the work by Butler et al. []. aryan et (199). Butler et al. (OP). E ojha and Hibbert (199), Lawrence (199). 'Cai and Pradhan (1993).

4 Transition Probabilities for the Dipole Allowed Fine Structure Transitions in S II 03 the CC calculations of Butler et al.; the present f-value is higher than the other calculations. The complete set of f-, S- and A-values for the dipole allowed fine structure transitions in SI1 obtained in the present work is presented in Table IV. The first line of each subset of data in the table corresponds to the LS transition, followed by the fine structure components. The degeneracy labels of the LS terms in the table correspond to those assigned in Table I1 for the energies. The energies of the initial and final levels in the fine structure set are given in unit of cm-, while the initial and the final LS states and the transitional energy differences are given in Rydberg units. The A-values are given in s-l, An asterisk () below an LS term in Table IV indicates an incomplete set of observed energy levels, and an asterisk for the energy corresponding to a transition indicates one or both of the levels missing from the set of observed energies. The table contains 1 fine structure transitions corresponding to 350 in LS coupling. The results obtained in the present work correspond to the 1 fine structure transitions among the 70 observed LS bound states of SII. This is comparatively a small fraction of the total number of possible fine structure transitions that can be processed among 31 calculated LS bound states. Based on accuracy of the calculated energies and comparison with other works, the accuracy of the present f-, S- and A-values should be within 15-0% for most of the transitions. It should however be noted that the present method obtains the fine structure components through pure algebraic transformation and does not consider any relativistic mixing of LS terms explicitly in the wavefunctions. This may result in higher uncertainty for transitions between highly excited levels where LSJ-mixing is significant. In that case the intercombination line could be strong enough to reduce the strengths of some of the dipole allowed lines, or shift the strengths among some fine structure components.. Conclusion Radiative transition probabilities for a large number of transitions in S I1 are presented. Observed energies are used in the transformation of the LS coupled transition matrix elements to fine structure for improved accuracy. As there are only a few experimental oscillator strengths available, a comprehensive evaluation of the theoretical data is difficult ; however there is good agreement with previous accurate theoretical calculations. The overall uncertainty due to relativistic effects for the dipole transitions should be small. However the transitions among highly excited levels may have higher uncertainty due to neglected mixing effects. Present results should provide a reasonably complete set of data for a large number of fine structure transitions in S 11. The entire table of transition probabilities and energies, Table IV, is available in electronic form from the author at: nahar@seaton.mps.ohio-state.edu, (a FORTRAN77 code is attached to the table to read the A-values and calculate the lifetimes). Acknowledgements I would like to thank Professor Anil K. Pradhan for comments and suggestions. This work was supported by NASA grants NAGW-3315 and NAS- 33. The computational work was carried out on the Cray YMP at the Ohio Supercomputer Center. References Osterbrock, D. E., Astrophysics of Gaseous Nebulae and Active Galactic Nuclei (University Science Books, Mill Valley, CA 199). Moos, W. et al., Astrophys. J. 3, L5 (1991). Wei Cai and Pradhan, A. K., Astrophys. J. Suppl.,39 (1993). Butler, K., Mendoza, C. and Zeippen, C.J., (to be published); data is. presently stored in the Opacity Project database, TOPbase, at CDS. Seaton, M. J., J. Phys. BU), 33 (197). Nahar, S. N., Physica Scripta,97 (1993). Nahar, S. N., Astron. Astrophys. 93, 33 (1995). Allen, C. W., Astrophysical Quantities (3rd Edition) (Athlone Press, London 197). Seaton, M. J., Yu, Y., Mihalas, D. and Pradhan, A. K., Mon. Not. R. Astron. Soc., 05 (199). Eissner, W., Jones, M. and Nussbaumer, H., Comput. Phys. Commun.,70 (197). Benington, K. A. et al., J. Phys. BZO, 379 (197). Martin, W. C., Zalubas, R., and Musgrove, A., J. Phys. Chem. Ref. Data 19, 1 (1990); Kaufman, V. and Martin, W. C., J. Phys. Chem. Ref. Data, 79 (1993). Ojha, P. C. and Hibbert, A., J. Phys. B, 1153 (199). Ryan, L. J., Rayburn, L. A. and Cunningham, A. J., J. Quant. Spectrosc. Radiat. Transfer,95 (199). Lawrence, G. M., Phys. Rev. 179,13 (199).

5 0 S. A. Nahar Table IV. The$, S- and A-vulues for transitions in S II E Ef Efi Transition cm-' cm-' RY S zs0-+ape B E -0.3B E O.Oo0 O.Oo B-01 7.E E E E B E E E-01 5.E E B+ 07 zso+b P' E E-01.0E E O.Oo E E B E-01 1.E-01.E -0.01E E B E+ 0 9.E E E E B E+09 O.Oo0 O.Oo0 O.Oo E E E E E E E E ES E ES E+ 09 zs0+d P" B E E-01.57B + 0 O.Oo0 O.Oo0 O.Oo E -0 1.E -0 7.B E E-01.50E-0.70B + 0.9E zs0+epc E E-01.E E E E E+00.5E E-01.3B-0.131E E E E E+09.70E + 09 z S0+f Pe E E E E+07 O.Oo0 O.Oo0 O.Oo E E E E B E B B E-0.1E+ 07.7E E +07 zs"-+gp' E E E E O.OO E E E+00.01E E -0.9E E-01.07E-01.E E E E+ 09 zso-+hp' B E E E-03.7E E E E-0.75B-03.3E E E E E E-01.5E O.Oo B E E E-0.37E E -0.79B E E- 0.39E+ 0.50E+0.55E E E -0.79B E+0 O.Oo0 O.Oo0 O.Oo E E E B-0 1.5B-0.E E E-0.5 1E- 0.55E + 0.5B + 0.0E + 0 y S0-+d Pc E E E+ 01.5E E E E E E E E E B E E + 07.E + 07 y s0+e Pc E E-01.1E E E- 01.7B-01.9B E - 01.E E B E E E B+0 1.9E + 0

6 Transition Probabilities for the Dipole Allowed Fine Structure Transitions in S II 05 Ei Er Efi ; Transition cm-1 cm-1 RY 9f 9, fir S S- ys"+fp' E E E E E E E E-0.57E -03.9E E E E E Ef0.93E+0 ys"-gpc E E E E ,39E E-01 3,1E E E-0 1.0E E E + 00.E E E E+07 y S"+h pc E E E E E E E E-03.0E E E-01.E-0.05E E+0 3.1E E+0 yso+ip' E E-0 1.0E + Do 1.70E E E E E E E E E E-01 1.E E E+07 yso+j p' E E E E E-01.3E E E E-03.51E-03.07E E E E E E+0 x S0-f Pc E E E E E E E E E-01.1E E+01.13E E E+0 5.1E E + 0 x S"+g P' E E E E E E E -0.59E E E E E E E E E +07 xs"+hp' E E E + 00.E E E E E E- 0.5E E le E E+ 0.13E+0.0 1E + 0 xso+ip' E E E E E E E-01.13E-0 5.E-0.73E E E+00.19E E E E + 07 xso+jpe E E E E E E E E E E E E E E E+0 a pc+ys E E E-01.7E E E E E-0 1.1E E E E E E E E+07 apc+xp E E-03.07E E s E E-01 A 9.57E E s E E E E E+07

7 0 S. A. Nahar Ei E, EJi Transition cm-' cm-' RY 9i gj fij a p0+z P E E -0 ap'+y P0 ape+zdo E E E-01.5E E-01.57E E E E E E E E E E-01.3E -01.E E-01.7E-01.17E E E E-01.31E E - 0.7E E E E E-0.5E E E E E E E E E-0.5E E E-07.NE E-05.35E-0.3E-05.5E-05 S 1.1E E E E E E E E E-01.E E -0.77E - 0.E-03.5E - 0.5E E E E E E E E E E E-0.3E E E E E E E + 07.E E E E E E E+07.05E Ec0.9E + 0.3E E+0.133Bf03.97E + 0.5E + 0.7E E E+0 ap'+yd" E E-0.997E E E E E E E E E E-01.7E E E E E-0.93E E E E -0.97E E-0.93E E E -0.97E-03.97E E + 0.E E E E+05.31E E E + 0 b Pe+ySo E E E E+0, E E E E E E E E E E E E+07 b pc+x s E E E E E-01.00E -01.5E E E E E E-0.099E E E E + 0 b Pe+zp E E E+01.E E E E E E E E E E E E E E E-0.53E E Ef00.1E+00.90E E E E E+07.7E E E E -k E + 07 bp"+ypo E E E-01.0E E E E E-01.30E E E E-03.3E E-0.0E E E - 03.E -0.51E E E E E-0 1.E-0 3.0E E E E E E E+0.0E + 05

8 Transition Probabilities for the Dipole Allowed Fine Structure Transitions in S II E E E E E E E E E E E-01 1.E E E E-0 3.MlE E-01.71E E-01.71E-01.93E E E + 00.E E E E E E+07.07E E E E E E E+07 b Pc+yDo E E-0.905E-0 3.E OE-01.75E E E-01.9E - 01.E E E- 01.7E-0.09E E E -0 1.E E E E-0 1.1E -0.1E E - 0. l00e E-03.1E -0.1E -03.1E E E E+0.15E E E E+05.59ESO5 cp'+ys" E E - 03.E E E E E E E E-0 1.3E+01 9.E+00.73E E+0.355Ei E+00 c PC+X s E E - 03.E-01.95E E-01.E E-01.57E-03.0E E E-01.E E E+0.97E E+ 0 cp"yp" E E E - 01.E E E-01.1E-01.39E-01.ME -01.7E E E E-03.3E E - 0.1E E E-0.735E E E E E E E E E E E E E+0.00E + 05 cp'+yd E E-03.1E E E - 01.E E-01.0E-01.30E E E E-01.30E E E E E-0 1.3E E E E E - 0.1E-03.53E-0.97E E E E-0.371Ef05.0E E E E E E+05.1E+05 dp'+xs" ME E E+ 0.E E E E E-01.0E E E E E ES 0.0E+0.3E + 0 d P'+ y P E E E+0 1.7E E E E-0.30E -0.50E -0.70E E E E-01.3E-01.30E - 0.1E E E-0 9.7E+01.17E E E E E E E+07.03E E+0.0E E E E+0

9 0 S. A. Nahar Ei E/ Eft, Transition cm-' cm-' RY 9i gf A/ S d P'+y Do E E E+0 1.3E E E E-0.00E OE E -0.00E E -0.75E E E-0 5.3E-01.37E E - 0.9OE-01.OE-01.03E E E+00 l.07e E+ 01.E E+Ol.3E E E E+05 1.WE E+ 0.1E+0.39E+0 1.1E E E-0 1.0E E E E E-0.E E -0 7.E E E+01.37E+01.03E E +OS 9.E E E Ef0 1.33E E E E-0 1.0E E OE E-0.33E-0.17E E- 0.57E -03.9E -0.9E E E+01.5E+01.5E E+00.E+01.E E E E +0.79E E+0 1M3E E E+ 0 ep"+ydo E E-05.99E-0 1.E E-0 1.0E E E-0.300E E E E E E- 0.0E E E E-07.99E - 0.1E E-0.5E E E E-03.E -0.1E E-03.3E E E E E E E E+ 00 a 'Da-a P E E-0 3.E+01.E E E E E E E E-01 1.E E-0.51E-0.19E E-0.39E E E - 0.5E-0 1.3E ES00 3.E E E E E+00.7E+00 1.E+ 07.E E E E E E E + 07 ad'-+ypo E E E E E E E E E E E E E E E E - 03.E E-0.09E E E E E E-01.09E-0 1.5E E-0.37E-0.595E E + 0.E E E+0 5.Et-05 5.E E+0 adc+zdo E E E E E E E E E E E E E E E E-03.E E E E E E E-0 1.1E E+ 00.1E- 01.1E E E E E E E E E+ 05.3E E+0 9.9E E E E+0 7.3E E+ 0

10 Transition Probabilities for the Dipole Allowed Fine Structure Transitions in S II 09 Transition E, an-' a De+y D E -01 Bi gr 0 0 ftr 3.0E -0 ; S S-.907E E E E E E E E E-01 3.E E-01 3.E-01.7E-0.55E E E-0 7.E E-0 1.7E-0 7.9E E E-0 1.3E E E -03.1E E E E -03.5E E E E E E+ 0.5E E E E E E E+ 05 b D'+yP" E E E +0.33E E-0.30E-0.E E E-0.00E -0.00E E E-01.3E E E E E E E E E E E E E E E+0 9.3E E E+0 1.7E E E+ 0.E+0 b D'+y Do E E E + 0.E E E E E E E E E E E E -0.70E E-0 3.E E -0.71E -0.37E E E E-0 3.E+01.19E E E E E E E E E+00.7E E+O5 1.17E E E E+05.3E E E E + 05 afe+zdo E E E E E E E E E E-01 1.E-01 1.E E E E E E -0.0E-0.351E-03.30E -0 3.E-0.05E-0.1E+01.E E E E E-01 9.E E E E E E+05.75E E E E E E+07 a F"+y D E E E E E-01.E E-01.53E-01.71E-01.3E-01.9E -01.1E-01.51E E E-0.05E E E E-0 5.E E-03.5E E E -0.5E E-01 7.E E-03.07E E E E E Ef E +07.9E E E+07.E E+07 bfe+ydo E E-01.9E UE E OE-0.90E -0.0E -0.30E E - 0.E E-0.30E E E - 0.7E-03.19E-01.77E -0 5.E E E E E E E E+0.51E E E E+01.9E E E E+ 0.1E E+0.599E + 0.5E E+0 5.1E+0

11 S. A. Nahar Transition Ei cm-' ZP0+Cpe 0.53 E f cm-' gf E E E+01.99E + 03 S E-03.00E E E E E E - 0.0E E-03.77E E E E E-03 1.E+Ol.5E+00.5E E t 00.53E+00.53E E E E+0.30E E E E + 03 z P"-.d Pe E E E E E E E E E E-01 1.E E E-0.999E-0.07E -0.0E E E ES E E E t E t E E f00.011es07.07e t E+07 7.E + 0.5E E E E E E E , E E-01.35E-01.3E E E E E E -0.70E-0.503E-0 1.9E E E E+00.01E E+00.0E E E-01.13E E E E E E le+ 07 zp"+fp' E E -0.71Et00.9E E E E E E E E E E E E E-0.1E-0.1E E-01.17E E E E E E E E t 0.91E+0.95E E E E+0 zp"+gp' E E E E E E E E E E E E E E-0.35E E-0.7E E E E E-01 1.E E E E-0.15E E t E Et0.7 15E E t E + 0 z P"+h P' E E-03.37E E E E E E E E E E E E E E E E E E E E-0 1.1E E -01.E-0.70E E Et E E E E E E E E E E E E-01.11E-01.1E -01.1E E E-03.79E E-03.39E-03.79E E E E E-01.09E E E-01.51E E E + 0.3E E E t 07.00E t 0.1E+0

12 Transition Probabilities for the Dipole Allowed Fine Structure Transitions in S II 11 Transition zpo,. JP c Ei cm-' E E E - 01.E E E E-01.E E E E E E E E-03 7.E E-01 1.E E E E E E E E E E+0.1E E E E E + 0 zpo+bd' E E E Ef E-01.9E -01.E-01.13E E E E E E E E-0.91E-01.51E E E E E E E E E E E E E E Ef0 1.E E+07.3E E E+0 z P0-x Da E E E E E E E E E E E E E E E-03.E-0.1E E E E-0.55E+ 00.E E E E E E E E ES E+0.9E E E E E + 07 zp"+dd' E E E E E E E E E E E E E E E E+00.5E E E E E E E E E E E E E Bf0.51Ef0.03E E + 07 z P0+e Dc E E E E E E-03 1 SE E E E E E-03.37E E E -0.37E E-01.1E E-0 5.3E E E E+0.175E E E E+M 1.0E E E+0 y P0-+f Pc E E E E yp"+gp' E-0 7.0E E E E E E E-0 9.7OE-0 9.0E E E E E E E E-0 1.0E E E-01.90E E -0.5E E E E E E-01.17E E E ES01.131E E E E E E E E E+01.5E E E E E E E E E E +0.07E E E E E+0.73E E E E + 0

13 1 S. A. Nahar Transition Ei an-' Efi RY 9i gf S y P"+h Pe E E E E E E E E E E E E l00e E E E E-0.1E E E E+00.11E E E E E+ 0.1E+0.1E + 0.0E+05 5.E + 0.1E E E E E E E E E E E E-01.9E E E E E E E E+00 1.E+00 1.E E E E E E+0 3.7E E E E E E+0 ypo+j pe E E - 0.7E E E E E E E E E E-0.1E E-03.00E E-03 1.E-0.503E E E E E E E E - 0.9E Ef0 1.35Ef0.090E E E E+05 yp"+c Dc E E E +O 3.539E E -0.90E -0.30E -0.9E-0.50E-0.E-0.70E -0.70E E E E-0.11E-01 3.E E-0.07E E ES E E E+01.55Et E E E E+0 1.5E+0. 19E E+07.0E E E + 07 ypo+dd' E E E E E E E E-0 1.5E-0.05E-03. 1E E E E-0 5.1E-0.97E E+00.7E +bo.97e E300.3E E-01.01E ES E E E E E E + 0.E E + 0 ypo+ed' E E E E - 0.1E E E - 0.0E E-0 1.3E E-0 1.3E-0.301E+00.51E E E E+00.7E E E E E E E+0.757E E+0.91E E+ 05.9E+0.59E+0 z D'+C Pc E E E Ef E-0.E E-0.30E E E-0.7E E E E E E E-0.37E E -0.5E-0.309E E E E-01.15E-0 9.E-03.11E-0.11E-0.1E E E E E E E E + 03

14 Transition Probabilities for the Dipole Allowed Fine Structure Transitions in S Transition Ei an-' Ef an-' zd"+dp' Eli RY.0E i gf fif Af; S S E E E E E-01.03E E E E E-01.1E -01.E E E E E E -0 1.E -01.5E E E E+ 01.9E E E E E+07.30E + 07.E E E+ 07.3E+0.001E+07.1E +07 zdo+epe QE E E E E E E E-01.55E E E-01.51E E E E - 0.1E E E E E E E E E E-01.E -0 1.E E E E+05 3.E E + 0.7E E+0 zd"+fp" E E - 0.7E E E-01 3.E E E-01 3.E E E E E -0.3E E E - 0.5E E -0.7E E E E E E E E E Et0 9.11E E E E+0.1E E + 07 zdo+gp' E E E E E E E-01 3.E E E E-01 1.E E -0.3E-05.71E-0.3E-0.09E E E-03.13E E -0.01E-03.E-0.177E E E E E $0 3.9E E E+0 7.5E E E E+0 zd"+hp E E E+ 00.3E E-01.10E E-01.13E E E E E E E E E-03 5.E E E-03.01E E E E E E E E E E+07.WE + 0.E E E E E+07 l.lloe + 07 z "Do+i Pc E E-0.53E -0 1.E E- 01.5E-01.75E-01.E E E-01.93E E E E -0.3E E-0.E E E E-0.09E E-03.53E E- 0.95E E E E-03.73E E E+ 0 7.E E E E E+05

15 1 S. A. Nahar A Ei El Eli S s-f; Transition cm-' cm-' RY Bi gr fir z~~+.j ~ c zdo+b Dc z ~o-c ~ e z~d"-+~~d~ Do' e De z D"+ b Fe E E E E - 01.E E -01.7E -01.1E -01.0E -01.1E -01.9E E-01.3E-01.7E-01.30E-01.99E E E-01.30E E E E E E E E E E E E E E-01.0E-01.01E-01.7E - 01.E-01.3E-01.5E E-01.57E-01.59OE E -01.1E -01.E E-01.19E E E E-01.1E E E - 0.3E E E E E-0 3.7E-05 9.ME E-0 1.7E E-01.07E - 0.7E-0.7E E E E E -0 7.E E E -0.09E E E E E E E E E OE E E -0.E-0.E E E E E-03.1E-03.15E E E-03.57E E E E -0.07E E E E E-0.1E E E-0.E E E-01.97E E E-01.1E E - 0 l.171e-0.3e E E E-03.79E-0.39E E E E+01.1E+00.1E ES00.73E E ES E E E+00.9E+00.50E E E E E E E E-01 1.E-01 1.E E E E-0 3.5E E E E-0.95E E E E -0.E -01.E E E - 0.E E E E E-0 1.3E-0 1.3E -0.17E+0.31E E E E E E E E E+01.0E E Ef E E E E E E E E Ef07.971E E+07.19E E E E E E E+07 1.E E E+0.E+0 5.7E+0 3.0E E E+0 3.7E E E+0 5.E E E E E E + 0.9E E E+0 3.0E E + 0.5E E E E E E E+0 1.5E+0 7.3E E + 0.E + 0.1E E E+0.093E+0 5.7Ef07.77E E+0.759E E+0