New Energy Levels of Doubly Ionized Manganese (Mn III (original) (raw)

The high resolution spectroscopy of manganese oxide

1989

This thesis reports studies of the electronic spectrum of gaseous MnO. The (0,0) band of the A 6 X + X 6 I + electronic transition of MnO was recorded by intermodulated laser-induced fluorescence over the range 17770 17970 cm 1 . The hyperfine structure caused by the 5 5 M n nucleus (I = 5/2) is almost completely resolved. Internal hyperfine perturbations between the F3 and F4 electron spin components (where N = J 1/2 and N = J + 1/2, respectively) occur in the ground state of MnO. These are caused by hyperfine matrix elements of the type AN = AF = 0, AJ = ± 1. Extra lines obeying the selection rules AJ = 0, ± 2 are also induced. Therefore, pCj34, RCj43, p 0 4 3 and R S 3 4 branches appear in the spectrum although they are not allowed in parallel transitions. The reason for the great complexity of the spectra is the occurrence of a large avoided crossing near N = 26 in the A 6 X + v = 0 level by another electronic state, B 6 Z + , with the same multiplicity and symmetry. The perturb...

On the Validity of the Spectator Electrons Model in the 3d and 4s Excitation Spectra of Mn I

Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences, 1979

New observations of the absorption spectrum of Mn I between 1800 and 700 Å have revealed 77 new transitions, arrangeable in Rydberg series converging on to experimentally known levels of the ion. The analysis of the spectrum at wavelengths shorter than 1300 Å suggests assignments for several previously unidentified transitions in the 1300-1600 Å range. Comparisons with ah initio Hartree-Fock calculations are attempted, and the spectator electrons model is shown to provide the correct framework for the analysis of 3d and 4s excitation in Mn I.

The influence of hyperfine structure on some manganese line profiles in the solar spectrum

Serbian Astronomical Journal, 2003

Taking into account effects of hyperfine structure, we calculated the synthetic solar spectrum for wavelength intervals around nine neutral manganese lines. To estimate values of hyperfine components we used the Oxford total absorption oscillator strength measurements (Booth et al. 1983). We compared observed profiles (Photometric Atlas of the Solar Spectrum from 3000 to 10000 ?(Delbouille et al. 1973)) of selected manganese lines with synthesized profiles in two cases: when hyperfine structure is not and when it is taken into account. By comparing the calculated with observed spectrum, we corrected the total oscillator strengths of all nine selected manganese lines.