Spectroscopic Studies of Extremely Metal‐poor Stars with the Subaru High‐Dispersion Spectrograph. IV. The α‐Element–Enhanced Metal‐poor Star BS 16934−002

2007/01/06 by Wako Aoki, Satoshi Honda, Timothy C. Beers +9 · 61 citations
Physics and Astronomy · #Abundance (ecology) #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Gamma-ray bursts and supernovae #Materials science #Metal #Metallurgy #Nucleosynthesis #Physics #Spectral line #Spectrograph #Star (game theory) #Stars #Stellar, planetary, and galactic studies #Supernova #astro-ph

paper · pdf · doi:10.1086/512601

published in The Astrophysical Journal 660(1), 747-761 (IOP Publishing) · 34 pages, 4 tables, 7 figures, Astrophysical Jounal, in press

arxiv created 2007/01/06 · openalex publication_date 2007/04/20 · arxiv updated 2011/02/11 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06

Abstract

A detailed elemental abundance analysis has been carried out for the very metal-poor ([Fe/H] = -2.7) star BS 16934-002, which was identified in our previous work as a star exhibiting large overabundances of Mg and Sc. A comparison of the abundance pattern of this star with that of the well-studied metal-poor star HD 122563 indicates excesses of O, Na, Mg, Al, and Sc in BS 16934-002. Of particular interest, no excess of C or N is found in this object, in contrast to CS 22949-037 and CS 29498-043, two previously known carbon-rich, extremely metal-poor stars with excesses of the α-elements. No established nucleosynthesis model exists that explains the observed abundance pattern of BS 16934-002. A supernova model, including mixing and fallback and assuming severe mass loss before explosion, is discussed as a candidate progenitor of BS 16934-002.

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