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

  • B. Barbuy (a1), M. Spite (a2), V. Hill (a3), F. Primas (a4), B. Plez (a5), R. Cayrel (a2), C. Sneden (a6), F. Spite (a2), T. C. Beers (a7), J. Andersen (a8), B. Nordström (a8), P. Bonifacio (a2), P. François (a2), P. Molaro (a9) and C. Siqueira-Mello (a1)...

Abstract

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.

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References

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Alvarez, R. & Plez, B. 1998, A&A, 330, 1109
Cayrel, R., Hill, V., Beers, T. C., Barbuy, B, Spite, M. et al. 2001, Nature, 409, 691
Hill, V., Plez, B., Cayrel, R., Beers, T. C., Nordström, B. et al. 2002, A&A, 387, 560
Plez, B., Hill, V., Cayrel, R., Spite, M., Barbuy, B. et al. 2004, A&A, 428, L9
Sneden, C., Preston, G. W., McWilliam, A., & Searle, L. 1994, ApJ, 431, L27
Toenjes, R., Schatz, H., Kratz, K.-L., Pfeiffer, B., Beers, T. C. et al. 2002, ASPC, 245, 376
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Keywords

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

  • B. Barbuy (a1), M. Spite (a2), V. Hill (a3), F. Primas (a4), B. Plez (a5), R. Cayrel (a2), C. Sneden (a6), F. Spite (a2), T. C. Beers (a7), J. Andersen (a8), B. Nordström (a8), P. Bonifacio (a2), P. François (a2), P. Molaro (a9) and C. Siqueira-Mello (a1)...

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