Hostname: page-component-78c5997874-v9fdk Total loading time: 0 Render date: 2024-11-10T14:19:49.809Z Has data issue: false hasContentIssue false
  • English
  • Français

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
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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

Alvarez, R. & Plez, B. 1998, A&A, 330, 1109Google Scholar
Cayrel, R., Hill, V., Beers, T. C., Barbuy, B, Spite, M. et al. 2001, Nature, 409, 691CrossRefGoogle Scholar
Hill, V., Plez, B., Cayrel, R., Beers, T. C., Nordström, B. et al. 2002, A&A, 387, 560Google Scholar
Plez, B., Hill, V., Cayrel, R., Spite, M., Barbuy, B. et al. 2004, A&A, 428, L9Google Scholar
Sneden, C., Preston, G. W., McWilliam, A., & Searle, L. 1994, ApJ, 431, L27CrossRefGoogle Scholar
Toenjes, R., Schatz, H., Kratz, K.-L., Pfeiffer, B., Beers, T. C. et al. 2002, ASPC, 245, 376Google Scholar