Very metal poor stars in the Milky Way:: constraints on stellar nucleosynthesis

被引：1

作者：

Chiappini, C

Matteucci, F

François, P

Cayrel, R

Spite, M

Spite, F

机构：

[1] Osserv Astron Trieste, INAF, Trieste, Italy

[2] Univ Trieste, Dept Astron, Trieste, Italy

[3] Observ Paris, F-75014 Paris, France

[4] Observ Paris, F-92195 Meudon, France

来源：

NUCLEAR PHYSICS A | 2005年 / 758卷

关键词：

D O I：

10.1016/j.nuclphysa.2005.05.040

中图分类号：

O57 [原子核物理学、高能物理学];

学科分类号：

070202 ;

摘要：

Recently Cayrel et al. [1] have derived the abundances of several a and Fe-peak elements for a sample of very metal poor giants ([Fe/H] from -4.0 to -3.0 dex) thus allowing us to test chemical evolution models in a metallicity range never reached before. Moreover, the small spread in the [el/Fe] ratios in the metallicity range from [Fe/H]=-4.0 up to -3.0 dex [1] is a clear sign that the halo of the Milky Way was well mixed even in the earliest phases of its evolution. We computed the evolution of the abundances of 0, Mg, Si, Ca, K, Ti, Sc, Ni, Mn, Co, Fe and Zn in the Milky Way. We made use of the most widely adopted nucleosynthesis calculations and compared the model results with observational data with the aim of imposing constraints upon stellar yields.

引用

页码：217C / 220C

页数：4

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