M. Swartz, S. O. Kastner, L. Goldsmith, and W. M. Neupert, "Observations of 3p53d–3p54f and 3p63d–3p53d4s transitions in iron, cobalt, nickel, and copper," J. Opt. Soc. Am. 66, 240-244 (1976)
Wavelengths of 3p53d–3p54f and 3p63d–3p53d4s transitions, in the range 60–120 Å, have been remeasured in iron, cobalt, nickel, and copper. In the former array, some additional transitions of singlet type are tentatively identified. For the latter array the present wavelengths differ by about 0.04 Å from values previously given in the literature for Nix.
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B. Edlén, Z. Physik 100, 621 (1936).
B. C. Fawcett, N. J. Peacock, and R. D. Cowan, J. Phys. B 1, 295 (1968).
W. E. Behring, L. Cohen, and U. Feldman, Astrophys. J. 175, 493 (1972); this solar wavelength differs from the earlier laboratory value of 89.104 Å given for the same line by Edlén [Z. Physik 104, 188 (1936)], but it gave somewhat better internal consistency in our calibration.
B. C. Fawcett, R. D. Cowan, E. Y. Kononov, and R. W. Hayes J. Phys. B 5, 1255 (1972).
E. Alexander, U. Feldman, and B. S. Fraenkel, J. Opt. Soc. Am. 55, 650 (1965).
U. Feldman, L. Katz, W. Behring, and L. Cohen, J. Opt. Soc. Am. 61, 91 (1971).
M. Even-Zohar and B. S. Fraenkel, J. Opt. Soc. Am. 58, 1420 (1968).
P. G. Kruger and F. S. Cooper, Phys. Rev. 44, 826 (1933).
TABLE II
Observed wavelengths (Å) and intensities of 3p53d–3p54f transitions.
Levels 3P1, 3D1, 1P1 obtained from resonance line wavelengths given by Svensson et al.4; other levels, except for 3P0 obtained in present work, derived from level intervals extrapolated by Svensson et al.4 (their Fig. 2). These values are considered accurate to within ±300 cm−1.
The 3p54f configuration is in J1l coupling rather than LS coupling; the number before the brackets gives the J value of the 3p5 core, while the number within the brackets gives the resultant K formed by coupling J1 with l of the outer electron.
Levels derived from present Fe ix 3p53d–3p54f wavelengths (Table II) coupled with 3p53d level values given by Svensson et al.4; these values are considered accurate to within ±200cm−1.
Levels derived from present Ni xi 3p53d–3p54f wavelengths (Table II) coupled with Ni xi 3p53d levels given in second column of this table. These values are considered accurate to within ±500 cm−1, except for the 1D2 level.
B. Edlén, Z. Physik 100, 621 (1936).
B. C. Fawcett, N. J. Peacock, and R. D. Cowan, J. Phys. B 1, 295 (1968).
W. E. Behring, L. Cohen, and U. Feldman, Astrophys. J. 175, 493 (1972); this solar wavelength differs from the earlier laboratory value of 89.104 Å given for the same line by Edlén [Z. Physik 104, 188 (1936)], but it gave somewhat better internal consistency in our calibration.
B. C. Fawcett, R. D. Cowan, E. Y. Kononov, and R. W. Hayes J. Phys. B 5, 1255 (1972).
E. Alexander, U. Feldman, and B. S. Fraenkel, J. Opt. Soc. Am. 55, 650 (1965).
U. Feldman, L. Katz, W. Behring, and L. Cohen, J. Opt. Soc. Am. 61, 91 (1971).
M. Even-Zohar and B. S. Fraenkel, J. Opt. Soc. Am. 58, 1420 (1968).
P. G. Kruger and F. S. Cooper, Phys. Rev. 44, 826 (1933).
TABLE II
Observed wavelengths (Å) and intensities of 3p53d–3p54f transitions.
Levels 3P1, 3D1, 1P1 obtained from resonance line wavelengths given by Svensson et al.4; other levels, except for 3P0 obtained in present work, derived from level intervals extrapolated by Svensson et al.4 (their Fig. 2). These values are considered accurate to within ±300 cm−1.
The 3p54f configuration is in J1l coupling rather than LS coupling; the number before the brackets gives the J value of the 3p5 core, while the number within the brackets gives the resultant K formed by coupling J1 with l of the outer electron.
Levels derived from present Fe ix 3p53d–3p54f wavelengths (Table II) coupled with 3p53d level values given by Svensson et al.4; these values are considered accurate to within ±200cm−1.
Levels derived from present Ni xi 3p53d–3p54f wavelengths (Table II) coupled with Ni xi 3p53d levels given in second column of this table. These values are considered accurate to within ±500 cm−1, except for the 1D2 level.