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A view of the Galactic halo using beryllium as a time scale

Published online by Cambridge University Press:  09 March 2010

Rodolfo Smiljanic
Affiliation:
IAG, Universidade de São Paulo, São Paulo, Brazil email: rsmiljan@eso.org
L. Pasquini
Affiliation:
ESO, Garching bei München, Germany
P. Bonifacio
Affiliation:
GEPI Observatoire de Paris - Meudon, France INAF, Osservatorio di Trieste, Trieste, Italy CIFIST Marie Curie Excellence Team
D. Galli
Affiliation:
INAF-Osservatorio di Arcetri, Firenze, Italy
B. Barbuy
Affiliation:
IAG, Universidade de São Paulo, São Paulo, Brazil email: rsmiljan@eso.org
R. Gratton
Affiliation:
INAF-Osservatorio di Padova, Padova, Italy
S. Randich
Affiliation:
INAF-Osservatorio di Arcetri, Firenze, Italy
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Abstract

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Beryllium stellar abundances were suggested to be a good tracer of time in the early Galaxy. In an investigation of its use as a cosmochronometer, using a large sample of local halo and thick-disk dwarfs, evidence was found that in a log(Be/H) vs. [α/Fe] diagram the halo stars separate into two components. One is consistent with predictions of evolutionary models while the other is chemically indistinguishable from the thick-disk stars. This is interpreted as a difference in the star formation history of the two components and suggests that the local halo is not a single uniform population where a clear age-metallicity relation can be defined.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2010

References

Fabbian, D., Asplund, M., Barklem, P. S., et al. 2009, A&A, 500, 1221Google Scholar
Nissen, P. E. & Schuster, W. J. 1997, A&A, 326, 751Google Scholar
Nissen, P. E. & Schuster, W. J. 2009, in: Proc. IAU Symposium No. 254, p. 103CrossRefGoogle Scholar
Pasquini, L., Bonifacio, P., Randich, S., Galli, D., & Gratton, R. G. 2004, A&A, 426, 651Google Scholar
Pasquini, L., Bonifacio, P., Randich, S., et al. 2007, A&A, 464, 601Google Scholar
Pasquini, L., Galli, D., Gratton, R. G., et al. 2005, A&A, 436, L57Google Scholar
Smiljanic, R., Pasquini, L., Bonifacio, P., et al. 2009, A&A, 499, 103Google Scholar
Suzuki, T. K. & Yoshii, Y. 2001, ApJ, 549, 303CrossRefGoogle Scholar
Valle, G., Ferrini, F., Galli, D., & Shore, S. N. 2002, ApJ, 566, 252CrossRefGoogle Scholar
Zolotov, A., Willman, B., Brooks, A. M., et al. 2009, ApJ, 702, 1058CrossRefGoogle Scholar