It is a well-established fact that the generation of the heavy elements occurred in stars—the Cauldrons of the Cosmos—via multiple complex nuclear reaction processes during stellar life and death. This paper will address the question of the first step, the formation of heavier elements such as carbon and oxygen from the primordial elemental abundance distribution in first stars. This nucleosynthesis can be facilitated by nuclear clustering of primordial isotopes in hot and highly convective first stars, provided that a helium rich or hydrogen depleted environment is available. The paper will summarize the associated nuclear reactions and the nucleosynthesis paths linking \(^4\)He to \(^{12}\)C. This will be based on an analysis of new experimental data for several of the anticipated nuclear reactions, and the role they might play at different temperature and density conditions in first star matter.

众所周知的事实是，重元素的产生是在恒星的生命和死亡过程中，通过多个复杂的核反应过程发生在恒星-宇宙的大锅中的。本文将讨论第一步的问题，即从第一颗恒星的原始元素丰度分布中形成较重的元素，例如碳和氧。只要存在富氦或贫氢的环境，原始核在热对流和高度对流的恒星中的核簇聚可以促进这种核合成。本文将总结相关的核反应和将\（^ 4 \） He与\（^ {12} \）链接的核合成路径。C.这将基于对一些预期核反应的新实验数据的分析，以及它们可能在第一恒星物质的不同温度和密度条件下发挥的作用。