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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 ,
L. Pasquini ,
P. Bonifacio ,
D. Galli ,
B. Barbuy ,
R. Gratton  and
S. Randich
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.

Keywords

stars: abundances – stars: late-type – Galaxy: halo
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. 134 - 135
Copyright
Copyright © International Astronomical Union 2010

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