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

Published online by Cambridge University Press:  09 March 2010

Hiroko Ito ,
Wako Aoki ,
Satoshi Honda ,
Timothy C. Beers  and
Nozomu Tominaga
Hiroko Ito
Affiliation:
Department of Astronomical Science, School of Physical Sciences, The Graduate University for Advanced Studies (SOKENDAI), 2-21-1, Osawa, Mitaka, Tokyo, 181-8588, Japan email: [email protected] National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
Wako Aoki
Affiliation:
Department of Astronomical Science, School of Physical Sciences, The Graduate University for Advanced Studies (SOKENDAI), 2-21-1, Osawa, Mitaka, Tokyo, 181-8588, Japan email: [email protected] National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
Satoshi Honda
Affiliation:
Gumma Astronomical Observatory, Agatsuma, Gunma, Japan
Timothy C. Beers
Affiliation:
Michigan State University, East Lansing, MI 48824-1116, USA
Nozomu Tominaga
Affiliation:
Konan University, Kobe, Hyogo, Japan
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Abstract

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We 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.

Keywords

stars: abundancesstars: individual(BD+44°493)stars: Population II
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 124 - 125
Copyright
Copyright © International Astronomical Union 2010

References

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