Astrophysics: How did the metals in a giant star originate?
Astrophysics: How did the metals in a giant star originate?
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天体物理学：巨星中的金属是如何起源的？
作者：
P. Bonifacio;M. Limongi;A. Chieffi
金属含量极低的恒星的化学成分（“金属”是指除氢和氦以外的所有元素）为我们提供了关于产生第一批金属的恒星质量的信息。然而，如果星星的表面已经被浓缩物质污染，这种直接的联系是不可能的，这些浓缩物质要么是从星星内部挖掘出来的，要么是从伴星星星转移过来的。在这里，我们认为，在HE 0107 -5240（参考文献）的情况下，已知的最贫铁的星星，氧丰度可能是一个判别：[O/Fe]比超过+3.5将有利于原始的金属起源，而[O/Fe]比小于+3将有利于污染假说。使用这个标准，我们建议如何获得所需的信息，氧丰度。
The chemical composition of stars with extremely low metal contents (taking 'metals' to mean all elements other than hydrogen and helium) provides us with information on the masses of the stars that produced the first metals. Such a direct connection is not possible, however, if the surface of the star has been polluted by enriched material, either dredged from the star's interior or transferred from a companion star. Here we argue that, in the case of HE0107–5240 (ref. ), the most iron-poor star known, the oxygen abundance could be a discriminant: a ratio of [O/Fe] exceeding +3.5 would favour a pristine origin of metals, whereas an [O/Fe] ratio of less than +3 would favour the pollution hypothesis. Using this criterion, we suggest how the required information on oxygen abundance might be obtained.