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.

引用

页码：122 / +

页数：2

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