Origin of the satellite Kβ 10 in X-ray spectra

Abstract

The transition energies corresponding to the transition array KM x → M x M 2,3 ( x = 1, 2, 3, 4, 5) have been calculated using Slater formulas for interaction between two holes in inner shells and HFS values of electrostatic Slater integrals. The initial and final state energies have been corrected for the adiabatic relaxation of atomic orbits, which take place due to creation of an inner vacancy. The value of this adiabatic relaxation energy for KM states has been calculated semi-empirically by comparing the KM 1 3 S 1→ L 3 M 1 3 P 2 transition energies with the measured Kα 1 line energies. For the final state, this value has been taken from available literature[21]. It is found that the satellite β 10 in the K-emission spectra of Zn, Ga, Ge, Mo and Rh is emitted by the superposition of more than one transition of the array. Consideration of the relative transition probabilities shows that the major contribution to β 10 comes from a K→ M 2,3 transition in the presence of a 3d spectator vacancy. It has been suggested that the satellite β′ 1 (7655.5 eV, Edamoto 1950) in the K-emission spectrum of cobalt, and the satellite β 7 (8271.2 eV) in the K-spectrum of nickel should be reidentified as β 10. It has been shown that the two lines β′ 1 (8268.0 eV) and β″ 1(8270.3 eV) observed[13] in the nickel Kβ spectrum are two components of the satellite β 10, and it is hence suggested that these should be renamed β 10 (1) and β 10 (2) respectively. Similarly, the lines β″ (1) (8909.3 eV) and β″ (2)(8913.0 eV) in the CuKβ spectrum are proved to be two components of β 10 and hence should be renamed β 10 (1) and β 10 (2) respectively.