Abstract

A theoretical analysis of the Eu i spectrum has been attempted with the use of available experimental data. Energy matrices including both electrostatic and spin–orbit interactions were constructed and, wherever possible, Slater parameters giving a best fit to the observed levels have been derived. The positions reported for terms below about 40 000 cm−1 arising from the addition of two electrons to the 8S7/2 ground state of the 4f7 core are critically examined. The analysis confirms the identifications previously given to terms below 32 000 cm−1 but reveals a number of discrepancies in the assignments of levels to higher terms. Tables of observed and computed wavenumbers, eigenvectors, and theoretical gJ values are presented for the configurations 4f7(8S)6s6p, 4f7(8S)6s5d, and 4f7(8S)5d6p. The configurations 4f7(8S)6s7s, 4f7(8S)6s8s, 4f7(8S)6s7p, 4f7(8S)6s5f, 4f7(8S)5d2, and 4f7(8S)6s6d are also discussed, together with the likely influence of configuration interaction. The analysis indicates the need for further experimental work before an understanding of these latter configurations can be achieved.

© 1965 Optical Society of America

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References

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  1. H. N. Russell and A. S. King, Astrophys. J. 90, 155 (1939).
    [CrossRef]
  2. P. G. Sandars and G. K. Woodgate, Proc. Roy. Soc. (London) A257, 269 (1960).
  3. H. N. Russell, W. Albertson, and D. N. Davis, Phys. Rev. 60, 641 (1941).
    [CrossRef]
  4. N. Zeldes, Phys. Rev. 90, 413 (1953).
    [CrossRef]
  5. G. Racah, J. Opt. Soc. Am. 50, 408 (1960).
  6. B. G. Wybourne, J. Math. Phys. 4, 354 (1963).
    [CrossRef]
  7. G. Racah, Physica 16, 651 (1950).
    [CrossRef]

1963 (1)

B. G. Wybourne, J. Math. Phys. 4, 354 (1963).
[CrossRef]

1960 (2)

G. Racah, J. Opt. Soc. Am. 50, 408 (1960).

P. G. Sandars and G. K. Woodgate, Proc. Roy. Soc. (London) A257, 269 (1960).

1953 (1)

N. Zeldes, Phys. Rev. 90, 413 (1953).
[CrossRef]

1950 (1)

G. Racah, Physica 16, 651 (1950).
[CrossRef]

1941 (1)

H. N. Russell, W. Albertson, and D. N. Davis, Phys. Rev. 60, 641 (1941).
[CrossRef]

1939 (1)

H. N. Russell and A. S. King, Astrophys. J. 90, 155 (1939).
[CrossRef]

Albertson, W.

H. N. Russell, W. Albertson, and D. N. Davis, Phys. Rev. 60, 641 (1941).
[CrossRef]

Davis, D. N.

H. N. Russell, W. Albertson, and D. N. Davis, Phys. Rev. 60, 641 (1941).
[CrossRef]

King, A. S.

H. N. Russell and A. S. King, Astrophys. J. 90, 155 (1939).
[CrossRef]

Racah, G.

G. Racah, J. Opt. Soc. Am. 50, 408 (1960).

G. Racah, Physica 16, 651 (1950).
[CrossRef]

Russell, H. N.

H. N. Russell, W. Albertson, and D. N. Davis, Phys. Rev. 60, 641 (1941).
[CrossRef]

H. N. Russell and A. S. King, Astrophys. J. 90, 155 (1939).
[CrossRef]

Sandars, P. G.

P. G. Sandars and G. K. Woodgate, Proc. Roy. Soc. (London) A257, 269 (1960).

Woodgate, G. K.

P. G. Sandars and G. K. Woodgate, Proc. Roy. Soc. (London) A257, 269 (1960).

Wybourne, B. G.

B. G. Wybourne, J. Math. Phys. 4, 354 (1963).
[CrossRef]

Zeldes, N.

N. Zeldes, Phys. Rev. 90, 413 (1953).
[CrossRef]

Astrophys. J. (1)

H. N. Russell and A. S. King, Astrophys. J. 90, 155 (1939).
[CrossRef]

J. Math. Phys. (1)

B. G. Wybourne, J. Math. Phys. 4, 354 (1963).
[CrossRef]

J. Opt. Soc. Am. (1)

G. Racah, J. Opt. Soc. Am. 50, 408 (1960).

Phys. Rev. (2)

H. N. Russell, W. Albertson, and D. N. Davis, Phys. Rev. 60, 641 (1941).
[CrossRef]

N. Zeldes, Phys. Rev. 90, 413 (1953).
[CrossRef]

Physica (1)

G. Racah, Physica 16, 651 (1950).
[CrossRef]

Proc. Roy. Soc. (London) (1)

P. G. Sandars and G. K. Woodgate, Proc. Roy. Soc. (London) A257, 269 (1960).

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Tables (3)

Tables Icon

Table I 4f7(8S)6s6p. G1(ps)=2701, X(fs)=210, X(fp)=84, ζp=1227, F0=19 771 cm−1.

Tables Icon

Table II 4f7(8S)6s5d. G2(ds)=1247, X(fs)=149, X(fd)=595, ζd=339, F0=19 834 cm−1.

Tables Icon

Table III 4f7(8S)5d6p. G1(dp)=460, G3(dp)=6, F2(dp)=198, X(fd)=698, X(fp)=91, ζd=454, ζp=673, F0=37 575 cm−1.

Equations (4)

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f 7 ( S 8 ) , ( l , l ) σ , λ ;             S , λ , J .
[ Σ ( O - C ) 2 / ( n - m ) ] 1 2 ,
f 7 ( S 8 ) l l ;             σ , λ i > j e 2 / r i j f 7 ( S 8 ) l l ;             σ , λ ,
f 7 ( S 8 ) l l ;             σ , λ i > j e 2 / r i j f 7 ( X ) l l ;             σ , λ .