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HEAVY-ELEMENT ABUNDANCES IN TWO SUBGIANT CH STARS
KALPANA KRISHNASWAMY and CHRISTOPHER SNEDEN
Publications of the Astronomical Society of the Pacific
Vol. 97, No. 591 (May 1985), pp. 407-417
Published by: Astronomical Society of the Pacific
Stable URL: http://www.jstor.org/stable/40678508
Page Count: 11
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New high-resolution, high signal-to-noise-ratio spectra have been gathered for subgiant CH stars HD 4395 and HD 216219. A detailed model-atmosphere abundance analysis has been carried out, with emphasis on the determination of abundances for elements heavier than iron. The heavy-element abundance patterns in the two stars are quite similar, and appear to have been produced by neutron exposures ( τ = 0.2) which are less than those in the typical classical barium star. The abundance patterns indicate that the source of neutrons could have been either the ¹³C(α,n)¹⁶ O reaction or the ²²Ne(α,n)²⁵ Mg reaction. The evolutionary states of these stars are rediscussed in light of these new results.
Publications of the Astronomical Society of the Pacific © 1985 The University of Chicago Press