Chemical evolution of r-process elements in the Draco dwarf spheroidal galaxy

被引：0
|
作者：
Ishigaki, M. N. [1 ]
Tsujimoto, T. [2 ]
Shigeyama, T. [3 ]
Aoki, W. [2 ]
机构：
[1] Univ Tokyo Kashiwanoha, Kavli Inst Phys & Math Universe, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan
[2] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan
[3] Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan
来源：
GENERAL ASSEMBLY OF GALAXY HALOS: STRUCTURE, ORIGIN AND EVOLUTION | 2016年 / 11卷 / S317期
关键词：
stars:abundances; galaxies:dwarf; galaxies:individual (Draco);
D O I：
10.1017/S1743921315009552
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
A dominant astrophysical site for r-process, which is responsible for producing heavy neutron-capture elements, is unknown. Dwarf spheroidal galaxies around the Milky Way halo provide ideal laboratories to investigate the origin and evolution of r-process elements. We carried out high-resolution spectroscopic observations of three giant stars in the Draco dwarf spheroidal galaxy to estimate their europium abundances. We found that the upper-limits of [Eu/H] are very low in the range [Fe/H]< -2, while this ratio is nearly constant at higher metallicities. This trend is not well reproduced with models which assume that Eu is produced together with Fe by SNe, and may suggest the contribution from other objects such as neutron-star mergers.
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页码：310 / 311
页数：2
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