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- W1521596516 abstract "Previous studies of visible-region high-excitation lines of Gaii in HgMn stars have usually concluded that these lines (4251-4262 and 6334) yield abundance estimates for gallium 1 dex greater than the UV resonance lines. Of the ex- planations proposed in the literature, we find that the presence of hyperfine structure (hfs) in the lines is the most likely. We analyse Lick Hamilton ´ Echelle CCD spectra by spectrum syn- thesis with the code UCLSYN. Using the Bidelman & Corliss (1962) measurements of hfs in Gaii, and the calculations given by Lanz et al. (1993), with the oscillator strengths by Ryabchi- kova & Smirnov (1994), we determine a difference in abundance (visual-UV) of only 0.2 dex. Of this difference, about 0.1 dex can be explained by the simplified approximation to the true hfs, which can be estimated theoretically, and the remaining 0.1 dex can probably be accounted for by the stratification of Ga found by Smith (1995, 1996b). We conclude that the visible- region and UV abundances are in agreement within the errors of the determinations, and that the anomaly previously found by several investigations is an artifact of the simplified atomic line structures assumed, or results from the use of very different gf-values from those adopted here." @default.
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- W1521596516 date "1998-05-01" @default.
- W1521596516 modified "2023-10-17" @default.
- W1521596516 title "The gallium problem in HgMn stars" @default.
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