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A very low upper limit for a Be abundance of a carbon-enhanced metal-poor star

Published online by Cambridge University Press:  23 April 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 1D LTE chemical abundance analysis of an extremely metal-poor star BD+44°493 ([Fe/H]= −3.7), and set a very low upper limit for its Be abundance: A(Be) < −2.0. It may indicate that the decreasing trend of Be abundances with lower [Fe/H] still holds at [Fe/H] < −3.5, and demonstrate that high C and O abundances do not necessarily imply high Be abundances. However, since the star is a subgiant with Teff ~ 5500K, Be may be depleted.

Keywords

stars: abundancesindividual (BD+44°493)Population II
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S268: Light Elements in the Universe , November 2009 , pp. 337 - 338
Copyright
Copyright © International Astronomical Union 2010

References

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