Abstract
The goal of this work is to obtain oscillator strengths (gf) of spectral lines of astrophysical interest. In addition, we aim to estimate the effects of the uncertainties associated with obtaining gf values in the calculation of stellar abundances. In the atmospheres of chemically peculiar stars, it is critical the accurate determination of the abundance of some chemical elements, as well as their possible variations with the time. With this in mind, we intend to analyze spectral lines observed in the spectrum of He-weak, He-strong, HgMn, and Ap stars. In this work we present some preliminary results we have obtained for XeII lines. We compare the gf values theoretically obtained, by adopting the Hartree-Fock (HF) method and the Least Square Fitting (LSF) approach, with the gf values empirically obtained. The astrophysical oscillator strengths for XeII lines obtained by Yuce et al (2011), by fitting observed spectra of xenon-overabundant stars with synthetic spectra, are considered as the empirical gf values in the present work.
