Detailed analyses of three neutron-capture-rich carbon-enhanced metal-poor stars

被引：0
|
作者：
Behara, N. T. [1 ,2 ]
Bonifacio, P. [1 ,2 ,3 ]
Ludwig, H. -G. [1 ,2 ]
Sbordone, L. [1 ,2 ]
Hernandez, J. I. Gonzalez [1 ,2 ]
Caffau, E. [2 ]
机构：
[1] CIFIST Marie Curie Excellence Team, Paris, France
[2] Univ Paris Diderot, CNRS, Observ Paris, GEPI, Paris, France
[3] Osserv Astron Trieste, Ist Nazl Astrofis, Trieste, Italy
来源：
CHEMICAL ABUNDANCES IN THE UNIVERSE: CONNECTING FIRST STARS TO PLANETS | 2010年 / 265期
关键词：
stars: abundances; stars: fundamental parameters; stars: AGB and post-AGB;
D O I：
10.1017/S1743921310000359
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Approximately 20% of very metal-poor stars ([Fe/H] < -2.0) are strongly enhanced in carbon ([C/Fe] > +1.0). Such stars are referred to as carbon-enhanced metal-poor (CEMP) stars. We present a chemical abundance analysis based on high resolution spectra acquired with UVES at the VLT of three dwarf CEMP stars: SDSS J1349-0229, SDSS J0912+0216 and SDSS J1036+1212. These very metal-poor stars, with [Fe/H] < -2.5, were selected from our ongoing survey of extremely metal-poor dwarf candidates from the SDSS. Among these CEMPs, SDSS J1349-0229 has been identified as a carbon star ([C/O] > +1.0). First and second peak r-process elements, as well as second peak r-process elements have been detected in all stars. In addition, elements from the third r-process peak were detected in one of the stars, SDSS J1036+1212. We present the abundance results of these stars in the context of neutron-capture nucleosynthesis theories.
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页码：122 / +
页数：2
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