Nuclear Heavy-ion Reactions in Stellar Fusion

该项目将发展量子力学理论，以描述恒星聚变反应的复杂过程，如12C + 12C。研究这种反应是了解超新星前大质量恒星中碳燃烧的关键。12C + 12C的聚变以共振增强为特征，部分原因在于12C + 12C体系中的分子态。萨里小组（物理学家）最近的工作。Rev. C 97, 055802)已经证明了时间相关波包方法解释一些共振行为的适用性。在这个项目中，我们将把这种方法与一个完全微观的理论（时间相关的生成器坐标方法）结合起来，以完善我们的理解，并包括聚类效应。通过将更微观的理论与计算效率更高的波包方法联系起来，我们将能够将该理论应用于远离稳定的原子核

This project will develop the quantum mechanical theories needed to describe the complex processes in stellar fusion reaction such as 12C + 12C. Studying such reactions is key to understand carbon burning in massive stars in pre-supernova phase. The fusion of 12C + 12C is characterized by resonant enhancement, in due part to molecular states in the 12C + 12C system. Recent work by the Surrey group (Phys. Rev. C 97, 055802) has demonstrated the applicability of a time-dependent wave packet approach to explaining some of the resonance behaviour. In this project, we will combine this approach with a fully microscopic theory (time-dependent generator coordinate method) to refine our understanding, and include clustering effects. By linking the more microscopic theory to the computationally-efficient wave packet method, we will be able to apply the theory to nuclei far from stability