Nuclear Heavy-ion Reactions in Stellar Fusion

该项目将发展描述恒星聚变反应（如12C + 12C）中复杂过程所需的量子力学理论。研究这种反应是理解大质量恒星在超新星爆发前阶段碳燃烧的关键。12C + 12C的熔合的特征在于共振增强，这部分归因于12C + 12C系统中的分子状态。最近的工作由萨里组（物理评论C 97，055802）已经证明了适用性的时间依赖波包的方法来解释一些共振行为。在这个项目中，我们将结合联合收割机这种方法与一个完全微观的理论（时间相关的发电机坐标方法），以完善我们的理解，并包括集群效应。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性的原子核

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