Abundances of neutron-capture elements in G 24-25. A halo-population CH subgiant

Details Abundances of neutron-capture elements in G 24-25. A halo-population CH subgiant Abundances of neutron-capture elements in G 24-25. A halo-population CH subgiant

2012-03-26

arxiv.org/abs/1203.5682v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

11 pages, 9 figures, accepted for publication in A&A

Scientific paper

10.1051/0004-6361/201117909

The differences between the neutron-capture element abundances of halo stars are important to our understanding of the nucleosynthesis of elements heavier than the iron group. We present a detailed abundance analysis of carbon and twelve neutron-capture elements from Sr up to Pb for a peculiar halo star G24-25 with [Fe/H] = -1.4 in order to probe its origin. The equivalent widths of unblended lines are measured from high resolution NOT/FIES spectra and used to derive abundances based on Kurucz model atmospheres. In the case of CH, Pr, Eu, Gd, and Pb lines, the abundances are derived by fitting synthetic profiles to the observed spectra. Abundance analyses are performed both relative to the Sun and to a normal halo star G16-20 that has similar stellar parameters as G24-25. We find that G24-25 is a halo subgiant star with an unseen component. It has large overabundances of carbon and heavy s-process elements and mild overabundances of Eu and light s-process elements. This abundance distribution is consistent with that of a typical CH giant. The abundance pattern can be explained by mass transfer from a former asymptotic giant branch component, which is now a white dwarf.

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