标题： 元素和同位素产率来自天琴座α星：预测和不确定性 显示英文标题

标题： Elemental and Isotopic Yields from T Coronae Borealis: Predictions and Uncertainties

摘要： T Coronae Borealis (T CrB) 是一个共生再发新星系统，预计将在未来两年内发生下一次爆发。 最近的流体动力学模拟预测了碳氧（CO）和氧氖（ONe）白矮星模型的核合成产率，但未考虑热核反应速率的不确定性。 我们基于2025年评估的更新后的热核反应速率和不确定性进行了详细的蒙特卡罗后处理核合成计算。 我们量化了结果的丰度不确定性，并确定了主导这些不确定性的关键核反应。 我们的结果表明，CO 和 ONe 新星模型都能稳健地产生特征性的 CNO 同位素。 对于质量数 A$\ge$20 的元素，丰度差异更为明显。 硫是区分 CO 和 ONe 新星模型最可靠的观测指标，其模型间差异为$\approx$30 倍，且对反应速率不确定性不敏感。 氖、硅和磷表现出更大的丰度差异（因子为$\approx$150-250），具有很强的诊断潜力。 尽管它们的预测产率受较大不确定性影响，但这些不确定性仍小于模型间的差异，使这些元素成为有用的、但精度较低的白矮星成分示踪剂。 氯、氩和钾在模型之间也存在差异，但 CO 和 ONe 模型的$\sigma$-丰度范围重叠，降低了它们作为成分示踪剂的当前实用性。 我们发现，只有九个核反应主导了最具诊断意义同位素的丰度不确定性，它们的影响在很大程度上独立于底层白矮星的组成。 这些结果为未来的实验工作以及解释 T CrB 下一次爆发的抛射物成分提供了指导。 显示英文摘要

摘要： T Coronae Borealis (T CrB) is a symbiotic recurrent nova system expected to undergo its next outburst within the next two years. Recent hydrodynamic simulations have predicted the nucleosynthetic yields for both carbon-oxygen (CO) and oxygen-neon (ONe) white-dwarf models, but without accounting for thermonuclear reaction-rate uncertainties. We perform detailed Monte Carlo post-processing nucleosynthesis calculations based on updated thermonuclear reaction rates and uncertainties from the 2025 evaluation. We quantify the resulting abundance uncertainties and identify the key nuclear reactions that dominate them. Our results show that both the CO and ONe nova models robustly produce characteristic CNO isotopes. More pronounced abundance differences emerge for elements with A $\ge$ 20. Sulfur is the most robust observational discriminator between the CO and ONe nova models, with a model-to-model difference of a factor of $\approx$30 and minimal sensitivity to reaction rate uncertainties. Neon, silicon, and phosphorus exhibit even larger abundance differences (factors of $\approx$150-250), providing strong diagnostic potential. While their predicted yields are subject to larger uncertainties, these remain smaller than the model-to-model differences, allowing these elements to serve as useful, though less precise, tracers of white-dwarf composition. Chlorine, argon, and potassium also differ between models, but the 1$\sigma$-abundance ranges for the CO and ONe models overlap, reducing their present usefulness as composition tracers. We find that only nine nuclear reactions dominate the abundance uncertainties of the most diagnostically important isotopes, and their influence is largely independent of the underlying white-dwarf composition. These results provide guidance for future experimental efforts and for interpreting ejecta compositions in the next eruption of T CrB.