arXivDaily arXiv每日学术速递 周一至周五更新
arXiv 2006.11208nucl-thastro-ph.SR
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$^{20}$ Ne分子的α聚类和α俘获反应速率

Alpha clustering and alpha-capture reaction rate from ab initio symmetry-adapted description of $^{20}$Ne

A. C. Dreyfuss, K. D. Launey, J. E. Escher, G. H. Sargsyan, R. B. Baker, T. Dytrych, J. P. Draayer

摘要:

我们介绍了一个新的框架,研究聚类和计算阿尔法部分宽度从头计算波函数。我们通过计算$^{16}$ O $+α$簇配置与从头算对称性适应无核壳模型中计算的$^{20}$ Ne中的状态之间的重叠,证明了$^{20}$ Ne的形式。我们提出了光谱振幅和光谱因子,并将其与更大模型空间中的无核辛壳模型结果进行比较,以深入了解驱动α-聚类的基本物理。具体而言,我们报告的最低$1^-$共振在$^{20}$氖,这是发现与实验吻合良好的α部分宽度。我们还提出了第一个无核壳模型估计的渐近归一化系数的基态,以及第一个兴奋的$4^{+}$状态的$^{20}$ Ne,在于在一个非常接近的$^{16}$ O $+α$阈值。这一结果突出了发展集群结构和描述阿尔法宽度的相关性的重要性。然后,宽度可以用来计算天体物理学感兴趣的窄共振的α捕获反应速率。我们探讨的反应速率的α-捕获反应$^{16}$ O $(α,γ)^{20}$ Ne在天体物理学相关的温度,并确定其对模拟X射线爆发丰度的影响。

英文摘要:

We introduce a new framework for studying clustering and for calculating alpha partial widths using ab initio wave functions. We demonstrate the formalism for $^{20}$Ne, by calculating the overlap between the $^{16}$O$+α$ cluster configuration and states in $^{20}$Ne computed in the ab initio symmetry-adapted no-core shell model. We present spectroscopic amplitudes and spectroscopic factors, and compare those to no-core symplectic shell-model results in larger model spaces, to gain insight into the underlying physics that drives alpha-clustering. Specifically, we report on the alpha partial width of the lowest $1^-$ resonance in $^{20}$Ne, which is found to be in good agreement with experiment. We also present first no-core shell-model estimates for asymptotic normalization coefficients for the ground state, as well as for the first excited $4^{+}$ state in $^{20}$Ne that lies in a close proximity to the $^{16}$O$+α$ threshold. This outcome highlights the importance of correlations for developing cluster structures and for describing alpha widths. The widths can then be used to calculate alpha-capture reaction rates for narrow resonances of interest to astrophysics. We explore the reaction rate for the alpha-capture reaction $^{16}$O$(α,γ)^{20}$Ne at astrophysically relevant temperatures and determine its impact on simulated X-ray burst abundances.

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