Lβ1 and Lβ2 Satellites in the X-ray Emission Spectra

Abstract

The X‐ray satellites Lβ1I, Lβ1II, Lβ1III, Lβ1IV, Lβ2I, Lβ2(b), Lβ2II and Lβ2(c) observed in the L‐emission spectra in elements with Z = 26 to 92, have been calculated. The energies of various transitions have been calculated by available Hartree‐Fock‐Slater (HFS) data using the semi‐empirical Auger transition energies in the doubly ionized atoms and their relative intensities have been estimated by considering cross ‐ sections of singly ionized 2x−1 (x ≡ s, p) states and then of subsequent Coster‐Kronig and shake off processes. The calculated spectra have been compared with the measured satellite energies in the L emission spectra. Their intense peaks have been identified as the observed satellite lines. The one to one correspondence between the peaks in calculated spectra and the satellites in measured spectra has been established on the basis of the agreement between the separations in the peak energies and those in the measured satellite energies. Group of transitions under the transition schemes L2Mx‐MxM4,5 and L3Mx‐MxN4,5 (x ≡ 1–5), which give rise to these satellites have been identified. It is observed that the satellite Lβ2(b) in all these spectra can be assigned to the superposition of 3F4‐3G5 and 3F4‐3D3 transitions and that this must be most intense one out of all these satellites, contributing in order of decreasing intensity. Each of the remaining satellites is found to have different origin in different elements. The possible contributions of the suitable transitions to all these lines have also been discussed.