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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: hiroko.ito@nao.ac.jp 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: hiroko.ito@nao.ac.jp 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

Boesgaard, A. M., Deliyannis, C. P., King, J. R., Ryan, S. G., et al. 1999 AJ, 117, 1549Google Scholar
Carney, B. W., Latham, D. W., Stefanik, R. P., Laird, J. B., & Morse, J. A. 2003, AJ, 125, 293CrossRefGoogle Scholar
Ito, H., Aoki, W., Honda, S., & Beers, T. C. 2009, ApJL, 698, L37Google Scholar
Meynet, G., Ekström, S., & Maeder, A. 2006, A&A, 447, 623Google Scholar
Nishimura, T., Aikawa, M., Suda, T., & Fujimoto, M. Y. 2009, accepted for PASJGoogle Scholar
Tominaga, N., Maeda, K., Umeda, H., Nomoto, K., et al. 2007, ApJL, 657, L77CrossRefGoogle Scholar