ON THE LINE SHIFTS AND OSCILLATOR STRENGTHS OF Xe II LINES IN THE SPECTRA OF HnMg STARS

DI ROCCO, HECTOR OSCAR; A. CRUZADO

ASTRONOMY AND ASTROPHYSICS

EDP SCIENCES S A

Lugar: Paris; Año: 2015 vol. 581

0004-6361

The ultimate goal that has motivated this work is to achieve realistic oscillator strength ( g f ) values to find reliable values ofstellar abundances. We aim to compare theg f valúes of Xeii lines found with di ff erent theoretical and experimental methods.Methods.We have undertaken calculations using the quasirelativistic and relativistic Hartree-Fock methods. Then we compare theseresults with those previously obtained from UVES spectra of HgMn stars.Results. 1) Our theoretical g f values are more realistic than those previously obtained for most lines. When we consider onlyunblended, isolated , relatively noise-free lines , however, our theoretical g f values and Yuce?s stellar values diff er little from eachother. 2) In a discussion of the origin of the previously observed discrepancy between the wavelengths of Xeii lines deducted fromstellar spectra and those published by National Institute of Standa rds and Technology (NIST), we conclude that stellar wavelengthscould be considered the standard wavelengths whenever the densities in stellar atmospheres are smaller than 1 ×