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Cambridge University Press (CUP), Proceedings of the International Astronomical Union, S265(5), p. 124-125, 2009

DOI: 10.1017/s1743921310000360

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The 9th Magnitude CEMP star BD+44°493: Origin of its Carbon Excess and Beryllium Abundance

Journal article published in 2009 by Hiroko Ito, Wako Aoki, Satoshi Honda, Timothy C. Beers, Nozomu Tominaga ORCID
This paper was not found in any repository, but could be made available legally by the author.
This paper was not found in any repository, but could be made available legally by the author.

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Abstract

AbstractWe performed a chemical abundance analysis of the very bright (V = 9.1) carbon-enhanced metal-poor (CEMP) star BD+44°493, which is the first star found with metallicity [Fe/H] < −3.5 and an apparent magnitude V < 12. The star is classified as a CEMP-no” subgiant, and its abundance pattern implies that a first-generation faint supernova is the most likely origin of its carbon excess. We set an very low upper limit on this star's beryllium abundance, which demonstrates that high C and O abundances do not necessarily imply high Be abundances.

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