In this work,the KLL dielectronic recombination (DR) processes of highly charged He-like to O-like xenon ions are studied systematically by using a DR program,which is based on the multi-configuration Dirac-Fock (MCDF) method.The KLL DR resonant energies and the corresponding resonant strengths are calculated,emphasizing especially the effect of the Breit interaction on the DR strengths.The theoretical KLL DR spectra are obtained and compared with the latest experimental results obtained in the Shanghai Electron Beam Ion Trap.
This paper calculates the electron impact excitation rate coefficients from the ground term 2s22p2 3P to the excited terms of the 2s22p2, 2s2p3, 2s22p3s, 2s22p3p, and 2s22p3d configurations of N II. In the calculations, multiconfiguration Dirac-Fork wave functions have been applied to describe the target-ion states and relativistic distorted-wave calculation has been performed to generate fine-structure collision strengths. The collision strengths are then averaged over a Maxwellian distribution of electron velocities in order to generate the effective collision strengths. The calculated rate coefficients are compared with available experimental and theoretical data, and some good agreements are found for the outer shell electron excitations. But for the inner shell electron excitations there are still some differences between the present calculations and available experiments.
The multi-configuration Dirac-Fock method is employed to calculate the transition energies,probabilities,and oscillator strengths for electric dipole allowed(E1) and forbidden(M1,E2,M2) lines for the 3s23p,3s3p2,3s23d,3p3,and 3s3p3d configurations of Fe XIV.The lifetimes of all 40 levels of these low-lying configurations are also derived.The valence-valence and core-valence correlation effects are accounted for in a systematic way.Breit interactions and quantum electrodynamics(QED) effects are estimated in subsequent relativistic configuration interaction(CI) calculations.The present results are in good agreement with other available theoretical and experimental values,and therefore can be used for the further astrophysical investigations.
