论文标题
建模$^{13} $ c中子源在AGB星星中的形成
Modeling the formation of the $^{13}$C neutron source in AGB stars
论文作者
论文摘要
AGB模型中不确定性的主要来源是氢的局部混合过程，这是形成所谓的$^{13} $ c口袋所必需的。在得出对这种物理过程的自洽处理的尝试中，有2D和3D模拟的磁性浮力模拟。由磁性浮力引起的混合而产生的$^{13} $ c口袋延伸到比迄今为止假设的区域大的区域，显示出几乎平坦的$^{13} $ c分布和可忽略的$^{14} $ n。最近，事实证明，它是匹配Presolar Sic Grains $ s $ emlements的同位素丰度比率的记录的好候选人。但是，最新的这种磁混合仅在后处理计算中应用，从未在恒星进化代码中实施。在这里，我们提出了新的恒星模型，该模型使用1-D静液压乐趣进化代码，其中包括磁性浮力。我们评论了由此产生的$ s $过程分布，并显示了与光谱观测和晶粒前测量值的初步比较。
A major source of uncertainty in AGB models is the partial-mixing process of hydrogen, required for the formation of the so-called $^{13}$C pocket. Among the attempts to derive a self-consistent treatment of this physical process, there are 2D and 3D simulations of magnetic buoyancy. The $^{13}$C pocket resulting from mixing induced by magnetic buoyancy extends over a region larger than those so far assumed, showing an almost flat $^{13}$C distribution and a negligible amount of $^{14}$N. Recently, it has been proved to be a good candidate to match the records of isotopic abundance ratios of $s$-elements in presolar SiC grains. However, up to date such a magnetic mixing has been applied in post-process calculations only, being never implemented in a stellar evolutionary code. Here we present new stellar models, performed with the 1-d hydrostatic FUNS evolutionary code, which include magnetic buoyancy. We comment the resulting $s$-process distributions and show preliminary comparisons to spectroscopic observations and pre-solar grains measurements.
