Hyperfine structure in the barium resonance line - Curves of growth for solar and r-process isotopic mixtures

Details Hyperfine structure in the barium resonance line - Curves of growth for solar and r-process isotopic mixtures Hyperfine structure in the barium resonance line - Curves of growth for solar and r-process isotopic mixtures

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...346.1030c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 346, Nov. 15, 1989, p. 1030-1034.

Astronomy and Astrophysics

Astrophysics

13

Fine Structure, Resonance Lines, Solar Spectra, Stellar Composition, Abundance, Barium, Dwarf Stars, Spectral Line Width, Stellar Atmospheres

Scientific paper

Equivalent widths of spectral lines of elements with even atomic numbers can be affected by hyperfine structures (hfs) in the isotopes with odd numbers of neutrons. We show that the most commonly studied line of the resonance doublet of barium, 4554 A is affected by hfs that could change the abundance by some 0.5 dex in unfavorable cases. The relative importance of hfs for this line is greater if the isotopic mix corresponds to the r-process. This might be the case in the oldest stars. Only modest changes in the generally accepted historical trend of r- to s-process abundances are expected when corrections for the hfs are made. Many barium determinations in old stars do not depend on the use of the 4554 A line. In any event, the errors introduced by neglect of hfs are of the same order as those due to uncertain damping, microturbulence, and non-LTE. The importance of blends, and the possibility of detecting the r-process isotopic mixture are discussed.

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