Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...141..362a&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 141, no. 2, Dec. 1984, p. 362-368. Research supported by The Citadel Developme
Astronomy and Astrophysics
Astrophysics
10
A Stars, Peculiar Stars, Stellar Composition, Stellar Spectra, Abundance, H Lines, Iron, Line Spectra, Metallic Stars
Scientific paper
The techniques used to derive the stellar temperatures and the elemental abundances of the cool Ap stars in Adelman's (1973) thesis are reassessed by using HD 8441 as an example. It is possible to find model atmospheres whose predictions match the H-gamma profile reasonably well in the line shoulder and the optical spectrophotometry outside of the regions obviously affected by the Ap star anomalies in an approximate manner. The final choice of stellar model is made by requiring that the Fe I and Fe II lines yield equal abundances and that the model's metallicity be comparable with the deduced abundances. For HD 8441, T(eff) = 9325 K and log g = 3.40, with iron being about three times the solar value. Of the elements with identified lines, chromium and heavier elements tend to be overabundant while carbon through vanadium tend to be underabundant.
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