Abundances in the Very Metal Poor s-Process-rich Star CS 22183-015

Details Abundances in the Very Metal Poor s-Process-rich Star CS 22183-015 Abundances in the Very Metal Poor s-Process-rich Star CS 22183-015

Nov 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...579l..87j&link_type=abstract

The Astrophysical Journal, Volume 579, Issue 2, pp. L87-L90.

Astronomy and Astrophysics

Astronomy

39

Subjeact Headings: Nuclear Reactions, Nucleosynthesis, Abundances, Stars: Abundances, Stars: Atmospheres

Scientific paper

We report on the abundances for 13 elements in CS 22183-015, the most metal-poor, s-process-rich star yet discovered. We measure [Fe/H]=-3.12 and large overabundances compared to scaled solar values for 11 heavy elements with s-process origin. The low luminosity of the star suggests that it is a CH star, a giant that has accreted s-processed material from an evolved, very metal poor companion. We find a [Pb/Ba] value of 1.1 dex and, more generally, that the ratio of heavy to light s-process elements is larger than seen in the solar system. This result is consistent with theoretical expectations for the s-process in metal-poor stars. [Eu/La] is higher than predicted from the solar system s-process abundance ratios. We argue that the s-process in metal-poor stars is more efficient at producing Eu that in asymptotic giant branch stars of solar metallicity. Data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.

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