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

  • Hiroko Ito (a1) (a2), Wako Aoki (a1) (a2), Satoshi Honda (a3), Timothy C. Beers (a4) and Nozomu Tominaga (a5)...

Abstract

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.

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References

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Boesgaard, A. M., Deliyannis, C. P., King, J. R., Ryan, S. G., et al. 1999 AJ, 117, 1549
Carney, B. W., Latham, D. W., Stefanik, R. P., Laird, J. B., & Morse, J. A. 2003, AJ, 125, 293
Ito, H., Aoki, W., Honda, S., & Beers, T. C. 2009, ApJL, 698, L37
Meynet, G., Ekström, S., & Maeder, A. 2006, A&A, 447, 623
Nishimura, T., Aikawa, M., Suda, T., & Fujimoto, M. Y. 2009, accepted for PASJ
Tominaga, N., Maeda, K., Umeda, H., Nomoto, K., et al. 2007, ApJL, 657, L77
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Keywords

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

  • Hiroko Ito (a1) (a2), Wako Aoki (a1) (a2), Satoshi Honda (a3), Timothy C. Beers (a4) and Nozomu Tominaga (a5)...

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