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  1. D. Desmarais and E. H. Pinnington, J. Opt, Soc. Am. 57, 1245 (1967).
  2. A. S. King, Astrophys. J. 72, 221 (1930).
  3. A. Y. Cabezas, I. Lindgren, and R. Marrus, Phys. Rev. 122, 1796 (1961).
  4. J. G. Conway and B. G. Wybourne, Phys. Rev. 130, 2325 (1963).
  5. W. F. Meggers, C. H. Corliss, and B. F. Scribner, Tables of Spectral Line Intensities, Natl. Bur. Std. (U.S.) Monograph 32— Part I (U.S. Govt. Printing Office, Washington, D.C., 1961).
  6. A. Gatterer and J. Junkes, Spektren der Selienen Erden (Specola Vaticana, Vatican, 1945).
  7. J. Sugar, J. Opt. Soc. Am. 58, 1519 (1968).
  8. J. H. McElaney, J. Opt. Soc. Am. 57, 870 (1967).
  9. Comparisons with other rare-earth spectra indicate that the 6s2 shell has little effect upon the 4ƒn configuration, and thus the ground multiplets for the first and third spectra are nearly identically spaced. Therefore, the ground-state 4I levels in Ho I should lie very close to the corresponding levels at 0, 5438, 8644, and 10770 cm-1 in Ho III. For Ho II, we obtain energies of 5750±50 and 6000±50 cm-1 for the second pair of levels, (13/2,½)7 and (13/2, ½)6, by interpolation between known levels in neighboring elements. This method forecasts the ground-state interval of 637.8 cm-1, to within ±20 cm-1.

Cabezas, A. Y.

A. Y. Cabezas, I. Lindgren, and R. Marrus, Phys. Rev. 122, 1796 (1961).

Conway, J. G.

J. G. Conway and B. G. Wybourne, Phys. Rev. 130, 2325 (1963).

Corliss, C. H.

W. F. Meggers, C. H. Corliss, and B. F. Scribner, Tables of Spectral Line Intensities, Natl. Bur. Std. (U.S.) Monograph 32— Part I (U.S. Govt. Printing Office, Washington, D.C., 1961).

Desmarais, D.

D. Desmarais and E. H. Pinnington, J. Opt, Soc. Am. 57, 1245 (1967).

Gatterer, A.

A. Gatterer and J. Junkes, Spektren der Selienen Erden (Specola Vaticana, Vatican, 1945).

Junkes, J.

A. Gatterer and J. Junkes, Spektren der Selienen Erden (Specola Vaticana, Vatican, 1945).

King, A. S.

A. S. King, Astrophys. J. 72, 221 (1930).

Lindgren, I.

A. Y. Cabezas, I. Lindgren, and R. Marrus, Phys. Rev. 122, 1796 (1961).

Marrus, R.

A. Y. Cabezas, I. Lindgren, and R. Marrus, Phys. Rev. 122, 1796 (1961).

McElaney, J. H.

J. H. McElaney, J. Opt. Soc. Am. 57, 870 (1967).

Meggers, W. F.

W. F. Meggers, C. H. Corliss, and B. F. Scribner, Tables of Spectral Line Intensities, Natl. Bur. Std. (U.S.) Monograph 32— Part I (U.S. Govt. Printing Office, Washington, D.C., 1961).

Pinnington, E. H.

D. Desmarais and E. H. Pinnington, J. Opt, Soc. Am. 57, 1245 (1967).

Scribner, B. F.

W. F. Meggers, C. H. Corliss, and B. F. Scribner, Tables of Spectral Line Intensities, Natl. Bur. Std. (U.S.) Monograph 32— Part I (U.S. Govt. Printing Office, Washington, D.C., 1961).

Sugar, J.

J. Sugar, J. Opt. Soc. Am. 58, 1519 (1968).

Wybourne, B. G.

J. G. Conway and B. G. Wybourne, Phys. Rev. 130, 2325 (1963).

Other

D. Desmarais and E. H. Pinnington, J. Opt, Soc. Am. 57, 1245 (1967).

A. S. King, Astrophys. J. 72, 221 (1930).

A. Y. Cabezas, I. Lindgren, and R. Marrus, Phys. Rev. 122, 1796 (1961).

J. G. Conway and B. G. Wybourne, Phys. Rev. 130, 2325 (1963).

W. F. Meggers, C. H. Corliss, and B. F. Scribner, Tables of Spectral Line Intensities, Natl. Bur. Std. (U.S.) Monograph 32— Part I (U.S. Govt. Printing Office, Washington, D.C., 1961).

A. Gatterer and J. Junkes, Spektren der Selienen Erden (Specola Vaticana, Vatican, 1945).

J. Sugar, J. Opt. Soc. Am. 58, 1519 (1968).

J. H. McElaney, J. Opt. Soc. Am. 57, 870 (1967).

Comparisons with other rare-earth spectra indicate that the 6s2 shell has little effect upon the 4ƒn configuration, and thus the ground multiplets for the first and third spectra are nearly identically spaced. Therefore, the ground-state 4I levels in Ho I should lie very close to the corresponding levels at 0, 5438, 8644, and 10770 cm-1 in Ho III. For Ho II, we obtain energies of 5750±50 and 6000±50 cm-1 for the second pair of levels, (13/2,½)7 and (13/2, ½)6, by interpolation between known levels in neighboring elements. This method forecasts the ground-state interval of 637.8 cm-1, to within ±20 cm-1.

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