56颗银河系核球红巨星中钴和铜的丰度
Cobalt and copper abundances in 56 Galactic bulge red giants
摘要：
银河系核球是银河系早期形成和化学富集的重要示踪物。场球星中不同铁峰元素的丰度可以提供有关最早期超新星核合成过程的信息。钴（Z=27）和铜（Z=29）是特别令人感兴趣的。我们的目标是确定核合成过程负责形成的铁峰元素Co和Cu。方法.我们在56颗球巨星中得到了铁峰元素钴和铜的丰度，其中13颗是红团簇星。我们的研究小组于2000-2002年在欧洲南方天文台甚大望远镜上使用FLAMES-UVES获得了高分辨率光谱，这似乎是迄今为止文献中获得的关于凸出红巨星的高分辨率数据的最高质量样本。多年来，我们已经推导出C、N、O、Na、Al、Mg、铁族元素Mn和Zn以及中子俘获元素的丰度。在目前的工作中，我们得出的铁峰元素钴和铜的丰度。我们还计算化学动力学演化模型来解释所观察到的这些元素的铁的功能的行为。样本星在所有金属丰度下的平均值为[Co/Fe]~0.0，当[Fe/H]>-0.8时，[Cu/Fe]~0.0，并随着次要元素的行为而向低金属丰度下降。我们得出结论，[Co/Fe]与[Fe/H]同步变化，这表明它应该是在大质量恒星富α冻结机制中产生的。相反，[Cu/Fe]遵循的行为，对较低的金属丰度的次要元素，表明其生产在弱的S-过程核合成在He燃烧和后期阶段。这里提出的化学动力学模型证实了这两种元素的行为（即[Co/Fe]与[Fe/H]~常数和[Cu/Fe]随着金属丰度的降低而降低）。
英文摘要：
The Milky Way bulge is an important tracer of the early formation and chemical enrichment of the Galaxy. The abundances of different iron-peak elements in field bulge stars can give information on the nucleosynthesis processes that took place in the earliest supernovae. Cobalt (Z=27) and copper (Z=29) are particularly interesting.We aim to identify the nucleosynthesis processes responsible for the formation of the iron-peak elements Co and Cu. Methods. We derived abundances of the iron-peak elements cobalt and copper in 56 bulge giants, 13 of which were red clump stars. High-resolution spectra were obtained using FLAMES-UVES at the ESO Very Large Telescope by our group in 2000-2002, which appears to be the highest quality sample of high-resolution data on bulge red giants obtained in the literature to date. Over the years we have derived the abundances of C, N, O, Na, Al, Mg; the iron-group elements Mn and Zn; and neutron-capture elements. In the present work we derive abundances of the iron-peak elements cobalt and copper. We also compute chemodynamical evolution models to interpret the observed behaviour of these elements as a function of iron. The sample stars show mean values of [Co/Fe]~0.0 at all metallicities, and [Cu/Fe]~0.0 for [Fe/H]>-0.8 and decreasing towards lower metallicities with a behaviour of a secondary element. We conclude that [Co/Fe] varies in lockstep with [Fe/H], which indicates that it should be produced in the alpha-rich freezeout mechanism in massive stars. Instead [Cu/Fe] follows the behaviour of a secondary element towards lower metallicities, indicating its production in the weak s-process nucleosynthesis in He-burning and later stages. The chemodynamical models presented here confirm the behaviour of these two elements (i.e. [Co/Fe] vs. [Fe/H]~constant and [Cu/Fe] decreasing with decreasing metallicities).
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