On the Galactic chemical evolution of sulfur

被引:42
作者
Ryde, N
Lambert, DL
机构
[1] Uppsala Astron Observ, S-75120 Uppsala, Sweden
[2] Univ Texas, Dept Astron, Austin, TX 78712 USA
关键词
stars : abundances; stars : atmospheres; stars : population II; Galaxy : abundances; Galaxy : evolution; Galaxy : halo;
D O I
10.1051/0004-6361:20034616
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Sulfur abundances have been determined for ten stars to resolve a debate in the literature on the Galactic chemical evolution of sulfur in the halo phase of the Milky Way. Our analysis is based on observations of the S I lines at 9212.9, 9228.1, and 9237.5 Angstrom for stars for which the S abundance was obtained previously from much weaker S I lines at 8694.0 and 8694.6 Angstrom. In contrast to the previous results showing [S/Fe] to rise steadily with decreasing [Fe/H], our results show that [S/Fe] is approximately constant for metal-poor stars ([Fe/H] less than or similar to-1) at [S/Fe]similar or equal to+0.3. Thus, sulfur behaves in a similar way to the other alpha elements, with an approximately constant [S/Fe] for metallicities lower than [Fe/H] similar or equal to-1. We suggest that the reason for the earlier claims of a rise of [S/Fe] is partly due to the use of the weak S I 8694.0 and 8694.6 Angstrom lines and partly uncertainties in the determination of the metallicity when using Fe I lines. The S I 9212.9, 9228.1, and 9237.5 Angstrom lines are preferred for an abundance analysis of sulfur for metal-poor stars.
引用
收藏
页码:559 / 569
页数:11
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