论文标题
早期旋转巨星的核合成和CEMP恒星的化学成分
Nucleosynthesis in early rotating massive stars and chemical composition of CEMP stars
论文作者
论文摘要
第一颗大型恒星通过释放宇宙中的第一金（比氦气重的元素）释放了化学演化的发作。这些恒星的性质以及早期化学富集的发生方式仍然在很大程度上未知。恒星内部旋转诱导的混合会影响巨大恒星恒星寿命期间的核合成，并导致具有各种化学成分的恒星喷射。我们提出了低和零金属性20、25和40 $ M _ {\ odot} $恒星模型，其核反应速率具有不同的初始旋转速率和假设。随着初始旋转的增加，光的产量（从$ \ sim $ c到al）和反铁元素被提高。核反应不确定性的影响很大。观察到的CEMP（碳增强金属贫困）的化学成分CS29528-028和HE0336+0113与材料的化学成分一致，该材料的化学成分是由40〜 $ M _ {\ odot} $模型弹出的材料的化学成分。
The first massive stars triggered the onset of chemical evolution by releasing the first metals (elements heavier than helium) in the Universe. The nature of these stars and how the early chemical enrichment took place is still largely unknown. Rotational-induced mixing in the stellar interior can impact the nucleosynthesis during the stellar life of massive stars and lead to stellar ejecta having various chemical compositions. We present low and zero-metallicity 20, 25 and 40 $M_{\odot}$ stellar models with various initial rotation rates and assumptions for the nuclear reactions rates. With increasing initial rotation, the yields of light (from $\sim$ C to Al) and trans-iron elements are boosted. The trans-iron elements (especially elements heavier than Ba) are significantly affected by the nuclear reaction uncertainties. The chemical composition of the observed CEMP (carbon-enhanced metal-poor) stars CS29528-028 and HE0336+0113 are consistent with the chemical composition of the material ejected by a fast rotating 40~$M_{\odot}$ model.
