研究快中子俘获核合成机制，分析太阳系r-过程元素丰度分布规律及其起源一直是原子核物理和天体物理等基础学科共同探讨的前沿课题之一。本项目拟结合动态r-过程理论模型，分析r-过程核合成元素的丰度分布，并将该丰度分布与经典模型的结果相比较，阐明r-过程动态模型局部的重要区域内再现太阳系r-过程元素丰度分布的优势（主要关注A~160附近的稀土氧化物区域）；基于原子核物理输入量的不确定性，在合理的数值变化范围内，探讨原子核物理的输入量（原子核质量和β衰变寿命）对r-过程元素丰度的具体影响；在N=80和N=126附近的重要区域内，利用各质量公式和理论模型来预言丰中子原子核的质量，并利用该预测的原子核质量进一步模拟计算r-过程元素的丰度。将模拟计算的结果与太阳系r-过程元素丰度的观测数据相比较，期望得到两者吻合效果最佳时的丰中子原子核质量的相互关系。

It has been one of the frontiers, in nuclear physics, astrophysics and some other basic disciplines, that studying the synthesis of heavy elements in the rapid neutron capture process (r-process) and analyzing the solar-system r-process elemental abundance distribution and its origin. This project aims to study the r-process elemental abundance distribution by using dynamic r-process simulations, and then compared with the results from classical r-process calculations, we show that dynamical r-process simulations can improve agreements with the solar r-process abundances in the important regions (mainly focus on the rare earth region of A~160); Considering the nondeterminacy of the nuclear physics input that play important roles in the r-process nucleosynthesis, we plan to research the sensitivity of the r-process abundances to the nuclear physics input (nuclear mass and beta-decay lifetime) with the corresponding data varied in a reasonable range; In the important regions of N=80 and N=126, a reliable theoretical predictions of the neutron-rich nuclear mass will be studied based on different nuclear mass models and relations, and then with these predicted nuclear masses we calculate the r-process elemental abundance in detail. Subsequently, we make a comparison between our results and the solar abundance observations to obtain a local mass relationship corresponding to the best agreement.