Heavy-element abundances in the classical barium star HR 774

Details Heavy-element abundances in the classical barium star HR 774 Heavy-element abundances in the classical barium star HR 774

Oct 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...273..722t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 273, Oct. 15, 1983, p. 722-741. Research supported by the Robert A. Welch F

Astronomy and Astrophysics

Astrophysics

94

Abundance, Barium, Heavy Elements, Metallic Stars, Stellar Spectra, Line Spectra, Neutrons, Nuclear Fusion, Spectrum Analysis, Tables (Data)

Scientific paper

Low-noise high-resolution Digicon and Reticon spectra of HR 774 are analyzed to determine abundances for all accessible heavy elements in the visual and near-infrared. The authors find evidence of departures from LTE as large as 0.5 dex affecting the low-excitation neutral lines of heavy elements in HR 774 and the standard star (β Gem). These severe effects cancel in a comparison of HR 774 with β Gem. Abundances of 19 heavy elements (Z ≥ 37) are determined and used to derive s-process overabundances. The predicted s-process abundances fit the derived s-process abundances remarkably well. The pattern of s-process abundances is consistent with the 13C(α, n)16O reaction as the neutron source and excludes the 22Ne(α, n)25Mg reaction.

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