R Coronae Borealis (RCB) stars are rare hydrogen-deficient carbon-rich variable supergiants thought to be the result of dynamically unstable white dwarf mergers. We attempt to model RCB stars through all the relevant timescales by simulating a merger event in Octo-tiger, a 3D adaptive mesh refinement (AMR) hydrodynamics code, and mapping the post-merger object into MESA, a 1D stellar evolution code. We then post-process the nucleosynthesis on a much larger nuclear reaction network to study the enhancement of s-process elements. We present models that match observations or previous studies in most surface abundances, isotopic ratios, early evolution, and lifetimes. We also observe similar mixing behavior to previous modeling attempts that result in the partial He-burning products visible on the surface in observations. However, we do note that our subsolar models lack any enhancement in s-process elements, which we attribute to a lack of hydrogen in the envelope. We also find that the ¹⁶O/¹⁸O isotopic ratio is very sensitive to initial hydrogen abundance and increases outside of the acceptable range with a hydrogen mass fraction greater than 10⁻⁴.

R Coronae Borealis (RCB) 恒星是稀有的缺氢富碳变超巨星，被认为是动态不稳定的白矮星合并的结果。我们试图通过在Octo-tiger 中模拟合并事件（一种 3D 自适应网格细化 (AMR) 流体动力学代码），并将合并后的对象映射到 MESA（一种 1D 恒星演化代码）中，通过所有相关的时间尺度对 RCB 恒星进行建模。然后，我们在更大的核反应网络上对核合成进行后处理，以研究s的增强- 过程元素。我们提供的模型与大多数表面丰度、同位素比率、早期演化和寿命方面的观察或先前研究相匹配。我们还观察到与先前建模尝试类似的混合行为，导致在观察中在表面上可见部分 He 燃烧产物。然而，我们确实注意到我们的太阳下模型在s 过程元素方面没有任何增强，我们将其归因于外壳中缺乏氢。我们还发现¹⁶ O/ ¹⁸ O 同位素比对初始氢丰度非常敏感，并且在氢质量分数大于 10 ^{-4 时}增加到可接受范围之外。