Astrophysical weak-interaction rates for selected A=20 and A=24 nuclei-猫眼课题宝

DOI：

10.1103/physrevc.89.045806

发表时间：

2014-02

期刊：

Physical Review C

影响因子：

3.1

通讯作者：

中科院分区：

物理与天体物理2区

文献类型：

作者：

G. Martínez-Pinedo;Y. Lam;K. Langanke;K. Langanke;R. Zegers;R. Zegers;C. Sullivan;C. Sullivan

我们用$M=8{M}_{\ensuremath{\bigodot}}$--12${M}_{\ensuremath{\bigodot}}$.计算了恒星演化后期温度和密度条件下的电子俘获率、衰减率和衰减率这些速率是基于最近的实验数据和大规模的壳模型计算得出的。我们证明了电子俘获率和衰减率都是基于这个天体物理范围内的数据的，除了在{20}和{24}上的俘获率外，其他的衰减率都是基于这个天体物理范围内的数据。我们预测它的主要贡献来自密度范围${log}_{10}\ensuremath{\rho}{Y}_{e}(\mathrm{g}\phantom{\rule{0.28em}{0ex}}{\mathrm{cm}}^{\ensuremath{-}3})=9.3$--9.6.中基态和{F}基态之间的第二禁戒跃迁少数个别跃迁的优势使我们能够在相关的天体物理条件下通过解析表达式表示不同的速率。我们还推导出了对速率的屏蔽修正。

We have evaluated the electron capture rates on $^{20}\mathrm{Ne}$, $^{20}\mathrm{F}$, $^{24}\mathrm{Mg}$, and $^{24}\mathrm{Na}$ and the $\ensuremath{\beta}$ decay rates for $^{20}\mathrm{F}$ and $^{24}\mathrm{Na}$ at temperature and density conditions relevant for the late-evolution stages of stars with $M=8{M}_{\ensuremath{\bigodot}}$--12${M}_{\ensuremath{\bigodot}}$. The rates are based on recent experimental data and large-scale shell-model calculations. We show that the electron capture rates on $^{20}\mathrm{Ne}$ and $^{24}\mathrm{Mg}$ and the $^{20}\mathrm{F}$ and $^{24}\mathrm{Na}$ $\ensuremath{\beta}$-decay rates are based on data in this astrophysical range, except for the capture rate on $^{20}\mathrm{Ne}$, which we predict to have a dominating contribution from the second-forbidden transition between the $^{20}\mathrm{Ne}$ and $^{20}\mathrm{F}$ ground states in the density range ${log}_{10}\ensuremath{\rho}{Y}_{e}(\mathrm{g}\phantom{\rule{0.28em}{0ex}}{\mathrm{cm}}^{\ensuremath{-}3})=9.3$--9.6. The dominance of a few individual transitions allows us to present the various rates by analytical expressions at the relevant astrophysical conditions. We also derive the screening corrections to the rates.

Astrophysical weak-interaction rates for selected A=20 and A=24 nuclei

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