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HST-STIS abundances in the uranium-rich very metal-poor star CS 31082-001

Published online by Cambridge University Press:  09 March 2010

B. Barbuy ,
M. Spite ,
V. Hill ,
F. Primas ,
B. Plez ,
R. Cayrel ,
C. Sneden ,
F. Spite ,
T. C. Beers  and
J. Andersen
...Show all authors
B. Barbuy
Affiliation:
Universidade de São Paulo, Brazil
M. Spite
Affiliation:
Observatoire de Paris, France
V. Hill
Affiliation:
Observatoire de la Côte d'Azur, France
F. Primas
Affiliation:
European Southern Observatory, Germany
B. Plez
Affiliation:
Université de Montpellier, France
R. Cayrel
Affiliation:
Observatoire de Paris, France
C. Sneden
Affiliation:
University of Texas, USA
F. Spite
Affiliation:
Observatoire de Paris, France
T. C. Beers
Affiliation:
Michigan State University, USA
J. Andersen
Affiliation:
Niels Bohr Institute, Denmark
B. Nordström
Affiliation:
Niels Bohr Institute, Denmark
P. Bonifacio
Affiliation:
Observatoire de Paris, France
P. François
Affiliation:
Observatoire de Paris, France
P. Molaro
Affiliation:
Osservatorio Astronomico di Trieste, Italy
C. Siqueira-Mello
Affiliation:
Universidade de São Paulo, Brazil
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Abstract

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The abundance derivation of heavy r-elements may provide a better understanding of the r-process, and the determination of several reference r-elements should allow a better determination of the star's age. The spatial ultraviolet (UV) region presents a large number of lines of heavy elements, and in some cases such as Bi, Pt, Au, detectable lines are only available in the UV. The extreme “r-process star” CS 31082-001 ([Fe/H] = −2.9) was observed in the spatial UV in order to determine abundances of the heavy elements, using STIS on board HST.

Keywords

metal-poor starsr-elementsultraviolet
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. 120 - 121
Copyright
Copyright © International Astronomical Union 2010

References

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