Abstract

Relative line strengths have been computed for the transition arrays of 3p54s–3p54p and 3p54s–3p55p in Ar i. Intermediate-coupling theory has been used, starting from LS coupling, and using the experimental energy levels as data for determining the parameters of the theory by least-squares adjustment of the calculated energies. The results have been placed on an absolute scale using the Coulomb approximation. The Landé g factors computed agree well with the observed values. The calculated transition probabilities are in fairly satisfactory agreement with various experimental determinations, and this agreement is better than that obtained using either LS- or jl-coupling calculations. The results for the 4s–4p array appear to be more accurate than those for the 4s–5p array.

© 1965 Optical Society of America

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  1. G. Racah, Phys. Rev. 61, 537 (1942).
  2. G. F. Koster and H. Statz, J. Appl. Phys. 32, 2054 (1961).
    [Crossref]
  3. H. Statz, C. L. Tang, and G. F. Koster, J. Appl. Phys. 34, 2625 (1963).
    [Crossref]
  4. W. L. Faust and R. A. McFarlane, J. Appl. Phys. 35, 2010 (1964).
    [Crossref]
  5. For example, R. H. Garstang, Mon. Not. Roy. Astron. Soc. 114, 118 (1954).
  6. E. U. Condon and G. H. Shortley, Theory of Atomic Spectra (Cambridge University Press, New York, 1952), pp. 298, 197, 268, 299.
  7. C. E. Moore, Natl. Bur. Std. Circ. U.S. No. 467, Vol.  1, 1949.
  8. Ref. 6, p. 385.
  9. Ref. 6, pp. 298, 299, 316.
  10. F. Rohrlich, Astrophys. J. 129, 449 (1959).
    [Crossref]
  11. D. R. Bates and A. Damgaard, Phil. Trans. Roy. Soc. (London) A242, 101 (1949).
  12. We have elected to use the Paschen notation for the energy levels, because we believe this makes comparison with other work easier. The pair-coupling notation may be found in Ref. 7.
  13. In one or two cases there was some uncertainty as to which LS-coupling level should be correlated with a given observed level. We adopted the guide that the LS-coupling level was the one which referred to the same diagonal-element position in the initial LS-coupling energy matrix that the calculated energy had in the final diagonal energy matrix.
  14. Ref. 6, p. 311.
  15. Formula (4) in Ref. 2 is correct as far as it goes, but it must be summed over the polarization index q, and hence multiplied by a factor 3, to give absolute line strengths. The same factor 3 must be applied to formulas (2.1) and (2.1a) of Ref. 3. Table IV of Ref. 3 is erroneous, and all entries in it must be multiplied by 4π/3, as must formula (2.2) of the same reference. See footnote 19 of Ref. 4 for further details.
  16. H. N. Olsen, J. Quant. Spectry. Radiative Transfer 3, 59 (1963).
    [Crossref]
  17. L. R. Doherty, thesis, University of Michigan (1961).
  18. A. P. Thorne and J. E. Chamberlain, Proc. Phys. Soc. (London) 82, 133 (1963).
    [Crossref]
  19. L. P. Razumovskaya, Opt. i Spektroskopiya 14, 189 (1963).[English transl.: Opt. Spectry. 14, 98 (1963).]
  20. W. E. Gericke, Z. Astrophys. 53, 68 (1961).
  21. H. W. Drawin, Z. Physik 146, 295 (1956).
    [Crossref]

1964 (1)

W. L. Faust and R. A. McFarlane, J. Appl. Phys. 35, 2010 (1964).
[Crossref]

1963 (4)

H. N. Olsen, J. Quant. Spectry. Radiative Transfer 3, 59 (1963).
[Crossref]

A. P. Thorne and J. E. Chamberlain, Proc. Phys. Soc. (London) 82, 133 (1963).
[Crossref]

L. P. Razumovskaya, Opt. i Spektroskopiya 14, 189 (1963).[English transl.: Opt. Spectry. 14, 98 (1963).]

H. Statz, C. L. Tang, and G. F. Koster, J. Appl. Phys. 34, 2625 (1963).
[Crossref]

1961 (2)

W. E. Gericke, Z. Astrophys. 53, 68 (1961).

G. F. Koster and H. Statz, J. Appl. Phys. 32, 2054 (1961).
[Crossref]

1959 (1)

F. Rohrlich, Astrophys. J. 129, 449 (1959).
[Crossref]

1956 (1)

H. W. Drawin, Z. Physik 146, 295 (1956).
[Crossref]

1954 (1)

For example, R. H. Garstang, Mon. Not. Roy. Astron. Soc. 114, 118 (1954).

1949 (2)

C. E. Moore, Natl. Bur. Std. Circ. U.S. No. 467, Vol.  1, 1949.

D. R. Bates and A. Damgaard, Phil. Trans. Roy. Soc. (London) A242, 101 (1949).

1942 (1)

G. Racah, Phys. Rev. 61, 537 (1942).

Bates, D. R.

D. R. Bates and A. Damgaard, Phil. Trans. Roy. Soc. (London) A242, 101 (1949).

Chamberlain, J. E.

A. P. Thorne and J. E. Chamberlain, Proc. Phys. Soc. (London) 82, 133 (1963).
[Crossref]

Condon, E. U.

E. U. Condon and G. H. Shortley, Theory of Atomic Spectra (Cambridge University Press, New York, 1952), pp. 298, 197, 268, 299.

Damgaard, A.

D. R. Bates and A. Damgaard, Phil. Trans. Roy. Soc. (London) A242, 101 (1949).

Doherty, L. R.

L. R. Doherty, thesis, University of Michigan (1961).

Drawin, H. W.

H. W. Drawin, Z. Physik 146, 295 (1956).
[Crossref]

Faust, W. L.

W. L. Faust and R. A. McFarlane, J. Appl. Phys. 35, 2010 (1964).
[Crossref]

Garstang, R. H.

For example, R. H. Garstang, Mon. Not. Roy. Astron. Soc. 114, 118 (1954).

Gericke, W. E.

W. E. Gericke, Z. Astrophys. 53, 68 (1961).

Koster, G. F.

H. Statz, C. L. Tang, and G. F. Koster, J. Appl. Phys. 34, 2625 (1963).
[Crossref]

G. F. Koster and H. Statz, J. Appl. Phys. 32, 2054 (1961).
[Crossref]

McFarlane, R. A.

W. L. Faust and R. A. McFarlane, J. Appl. Phys. 35, 2010 (1964).
[Crossref]

Moore, C. E.

C. E. Moore, Natl. Bur. Std. Circ. U.S. No. 467, Vol.  1, 1949.

Olsen, H. N.

H. N. Olsen, J. Quant. Spectry. Radiative Transfer 3, 59 (1963).
[Crossref]

Racah, G.

G. Racah, Phys. Rev. 61, 537 (1942).

Razumovskaya, L. P.

L. P. Razumovskaya, Opt. i Spektroskopiya 14, 189 (1963).[English transl.: Opt. Spectry. 14, 98 (1963).]

Rohrlich, F.

F. Rohrlich, Astrophys. J. 129, 449 (1959).
[Crossref]

Shortley, G. H.

E. U. Condon and G. H. Shortley, Theory of Atomic Spectra (Cambridge University Press, New York, 1952), pp. 298, 197, 268, 299.

Statz, H.

H. Statz, C. L. Tang, and G. F. Koster, J. Appl. Phys. 34, 2625 (1963).
[Crossref]

G. F. Koster and H. Statz, J. Appl. Phys. 32, 2054 (1961).
[Crossref]

Tang, C. L.

H. Statz, C. L. Tang, and G. F. Koster, J. Appl. Phys. 34, 2625 (1963).
[Crossref]

Thorne, A. P.

A. P. Thorne and J. E. Chamberlain, Proc. Phys. Soc. (London) 82, 133 (1963).
[Crossref]

Astrophys. J. (1)

F. Rohrlich, Astrophys. J. 129, 449 (1959).
[Crossref]

J. Appl. Phys. (3)

G. F. Koster and H. Statz, J. Appl. Phys. 32, 2054 (1961).
[Crossref]

H. Statz, C. L. Tang, and G. F. Koster, J. Appl. Phys. 34, 2625 (1963).
[Crossref]

W. L. Faust and R. A. McFarlane, J. Appl. Phys. 35, 2010 (1964).
[Crossref]

J. Quant. Spectry. Radiative Transfer (1)

H. N. Olsen, J. Quant. Spectry. Radiative Transfer 3, 59 (1963).
[Crossref]

Mon. Not. Roy. Astron. Soc. (1)

For example, R. H. Garstang, Mon. Not. Roy. Astron. Soc. 114, 118 (1954).

Natl. Bur. Std. Circ. U.S. No. 467 (1)

C. E. Moore, Natl. Bur. Std. Circ. U.S. No. 467, Vol.  1, 1949.

Opt. i Spektroskopiya (1)

L. P. Razumovskaya, Opt. i Spektroskopiya 14, 189 (1963).[English transl.: Opt. Spectry. 14, 98 (1963).]

Phil. Trans. Roy. Soc. (London) (1)

D. R. Bates and A. Damgaard, Phil. Trans. Roy. Soc. (London) A242, 101 (1949).

Phys. Rev. (1)

G. Racah, Phys. Rev. 61, 537 (1942).

Proc. Phys. Soc. (London) (1)

A. P. Thorne and J. E. Chamberlain, Proc. Phys. Soc. (London) 82, 133 (1963).
[Crossref]

Z. Astrophys. (1)

W. E. Gericke, Z. Astrophys. 53, 68 (1961).

Z. Physik (1)

H. W. Drawin, Z. Physik 146, 295 (1956).
[Crossref]

Other (8)

Ref. 6, p. 385.

Ref. 6, pp. 298, 299, 316.

L. R. Doherty, thesis, University of Michigan (1961).

We have elected to use the Paschen notation for the energy levels, because we believe this makes comparison with other work easier. The pair-coupling notation may be found in Ref. 7.

In one or two cases there was some uncertainty as to which LS-coupling level should be correlated with a given observed level. We adopted the guide that the LS-coupling level was the one which referred to the same diagonal-element position in the initial LS-coupling energy matrix that the calculated energy had in the final diagonal energy matrix.

Ref. 6, p. 311.

Formula (4) in Ref. 2 is correct as far as it goes, but it must be summed over the polarization index q, and hence multiplied by a factor 3, to give absolute line strengths. The same factor 3 must be applied to formulas (2.1) and (2.1a) of Ref. 3. Table IV of Ref. 3 is erroneous, and all entries in it must be multiplied by 4π/3, as must formula (2.2) of the same reference. See footnote 19 of Ref. 4 for further details.

E. U. Condon and G. H. Shortley, Theory of Atomic Spectra (Cambridge University Press, New York, 1952), pp. 298, 197, 268, 299.

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Tables (7)

Tables Icon

Table I Ar I adopted parameters (cm−1).

Tables Icon

Table II Ar i adopted parameters (cm−1).

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Table III Ar i energy levels (cm−1) in the 3p54s configuration.

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Table IV Ar i energy levels (cm−1).

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Table V Landé g factors in Ar i.

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Table VI Transition probabilities for the 4s–4p array of Ar i.

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Table VII Transition probabilities for the 4s–5p array of Ar i.