论文标题
在12C（α，γ）16o反应速率中的不确定性对低至中质量恒星的演变的影响
The impact of the uncertainties in the 12C(α,γ)16O reaction rate on the evolution of low- to intermediate-mass stars
论文作者
论文摘要
恒星进化计算中最大的不确定性之一是被考虑的反应速率的准确性。 12C（Alpha，Gamma）16o反应对于研究低质量和中间质量恒星的研究尤其重要，因为它决定了核心中最终的C/O比，从而影响了白矮人冷却演化。因此，需要研究迄今为止制造的白矮人及其祖细胞的计算如何受到12C（Alpha，Gamma）16o反应速率的不确定性的影响。在这项工作中，我们使用具有0.90 <= mi/msun范围的初始质量的MESA代码来计算完全进化序列。我们考虑从文献获得的不同的反应率以及其不确定性中的极端限制。正如预期的那样，我们发现，在核心氦燃烧阶段之前，恒星的演变没有变化。但是，随后的阶段都受到考虑的反应速率的不确定性的影响。特别是，我们发现在核心氦燃烧阶段与对流核心质量的差异，这可能会影响细分的脉冲特性，渐近巨型分支期间的热脉冲数量以及核心中最终氧丰度与残留白木源的祖细胞之间的趋势。
One of the largest uncertainties in stellar evolutionary computations is the accuracy of the considered reaction rates. The 12C(alpha,gamma)16O reaction is particularly important for the study of low- and intermediate-mass stars as it determines the final C/O ratio in the core which influences the white dwarf cooling evolution. Thus, there is a need for a study of how the computations of white dwarfs and their progenitors that are made to date may be affected by the uncertainties of the 12C(alpha,gamma)16O reaction rates. In this work we compute fully evolutionary sequences using the MESA code with initial masses in the range of 0.90 <= Mi/Msun <= 3.05. We consider different adopted reaction rates, obtained from the literature, as well as the extreme limits within their uncertainties. As expected, we find that previous to the core helium burning stage there are no changes to the evolution of the stars. However, the subsequent stages are all affected by the uncertainties of the considered reaction rate. In particular, we find differences to the convective core mass during the core helium burning stage which may affect pulsation properties of subdwarfs, the number of thermal pulses during the asymptotic giant branch and trends between final oxygen abundance in the core and the progenitor masses of the remnant white dwarfs.
