C01 LΑ Satellites in X-ray Emission Spectra of Elements 41Nb, 45Rh, 47Ag and 49In

Poonia, Surendra

doi:10.1154/1.1755162

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“…The detailed method of calculation of transition probabilities and their distribution have been presented in earlier papers. [3,[9][10][11][12][13][14][15][16]…”

Section: Transition Energiesmentioning

confidence: 99%

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Lβ₂ satellites in the X‐ray emission spectra of elements ₇₂Hf, ₇₃Ta, ₇₄W, ₈₁Tl, ₈₃Bi and ₉₂U

Poonia

2011

X-Ray Spectrometry

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The satellite spectra arising due to the L 3 M x -M x N 4,5 (x = 1-5) transition array in the X-ray emission spectra of 72 Hf, 73 Ta, 74 W, 81 Tl, 83 Bi and 92 U have been calculated using available HFS data on K-LM and L-MN Auger transition energies. The agreement between the calculated and measured energies, that between calculated and measured separations in energies and the consideration of the relative probabilities of all the L 3 M x -M x N 4,5 transitions have been used as the basis for deciding the origin of the satellites. It has been established that two satellites observed in the Lb 2 region of the X-ray spectra of various elements, named b 2 I and b 2 II in the order of increasing energy, are mainly emitted by the L 3 M 4,5 -M 4,5 N 4,5 transitions. It is observed that satellite b 2 I in the spectra of elements with 72 Hf to 74 W has been assigned to the superposition of the 3 F 4 -3 G 5 and 3 F 4 -3 D 3 transitions and must be the most intense one among all these satellites. The same transition has been proved to be the main origin of satellite b 2 II , reported in the element with 81 Tl, 83 Bi and 92 U. Further, satellite b 2 I , reported in the spectra of elements with 81 Tl and 92 U, has been associated with the transitions 3 D 3 -3 F 4 and 1 D 2 -1 F 3 . Finally, line b 2 II , reported in the spectra of elements with Z = 72-74, has been assigned to the 1 F 3 -1 G 4 and 3 P 0 -3 D 1 transitions. The possible contributions of other transitions of the L 3 M x -M x N 4,5 (x = 1-5) array having intensities comparable with those of the above transitions, as well as the corresponding lines that have not yet been observed, have also been discussed.

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“…The detailed method of calculation of transition probabilities and their distribution have been presented in earlier papers. [3,[9][10][11][12][13][14][15][16]…”

Section: Transition Energiesmentioning

confidence: 99%

“…This additional vacancy is created by the shaking of the atomic orbits due to a sudden change in the potential field in the atom, which takes place when a 2p 3/2 electron leaves the atom with a fast speed. The detailed method of calculation of transition probabilities and their distribution have been presented in earlier papers …”

Section: Calculationmentioning

confidence: 99%

Lβ₂ satellites in the X‐ray emission spectra of elements ₇₂Hf, ₇₃Ta, ₇₄W, ₈₁Tl, ₈₃Bi and ₉₂U

Poonia

2011

X-Ray Spectrometry

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C01 LΑ Satellites in X-ray Emission Spectra of Elements ₄₁Nb, ₄₅Rh, ₄₇Ag and ₄₉In

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Lβ₂ satellites in the X‐ray emission spectra of elements ₇₂Hf, ₇₃Ta, ₇₄W, ₈₁Tl, ₈₃Bi and ₉₂U

Lβ₂ satellites in the X‐ray emission spectra of elements ₇₂Hf, ₇₃Ta, ₇₄W, ₈₁Tl, ₈₃Bi and ₉₂U

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C01 LΑ Satellites in X-ray Emission Spectra of Elements 41Nb, 45Rh, 47Ag and 49In

Cited by 1 publication

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Lβ2 satellites in the X‐ray emission spectra of elements 72Hf, 73Ta, 74W, 81Tl, 83Bi and 92U

Lβ2 satellites in the X‐ray emission spectra of elements 72Hf, 73Ta, 74W, 81Tl, 83Bi and 92U

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C01 LΑ Satellites in X-ray Emission Spectra of Elements ₄₁Nb, ₄₅Rh, ₄₇Ag and ₄₉In

Lβ₂ satellites in the X‐ray emission spectra of elements ₇₂Hf, ₇₃Ta, ₇₄W, ₈₁Tl, ₈₃Bi and ₉₂U

Lβ₂ satellites in the X‐ray emission spectra of elements ₇₂Hf, ₇₃Ta, ₇₄W, ₈₁Tl, ₈₃Bi and ₉₂U