20个最重要的A < 65的fp壳层核的恒星弱作用率与质量丰度
Stellar Weak Rates and Mass Fractions of 20 Most Important $fp$-shell Nuclei with $A < 65$
AI总结：
本文计算了20个A<65的fp壳层核在恒星前超新星演化中的质量丰度与弱作用率，采用Sahas方程和pn-QRPA模型，并与独立粒子模型及大尺度壳模型进行比较，为恒星演化和超新星模拟提供更可靠的数据。
摘要：
本文给出了大质量恒星前超新星演化近期研究中20个最重要的A < 65电子俘获（ec）和β衰变（bd）核的恒星弱作用率与质量丰度。这些核的质量丰度利用Sahas方程计算，该方程假设核统计平衡，并采用一组代表大质量恒星中心区域在硅核燃烧后所经历轨迹的初始条件（$T_9$、$ρ$和$Y_e$）。我们计算的质量丰度在大多数情况下与独立粒子模型结果相比具有较好的可比性，并注意到最大可达4倍的差异。弱相互作用（ec和bd）速率采用完全微观的方式计算，使用质子-中子准粒子随机相位近似（pn-QRPA）模型，且未假设Brink-Axel假说。速率在密度范围（$10$-$10^{11}$）g/cm$^3$和温度范围（0.01-30）GK内计算。与大尺度壳模型相比，我们计算的速率在核心温度较高时更大。当前研究可能有助于更真实地模拟恒星演化过程和模拟核心坍缩超新星。
英文摘要：
This work presents stellar weak rates and mass fractions of 20 most important electron capture (ec) and beta decay (bd) nuclei with $A < 65$ according to a recent study during the presupernova evolution of massive stars. The mass fractions of these nuclei were calculated using the Sahas equation which assumes nuclear statistical equilibrium for a set of initial conditions ($T_9$, $ρ$ and $Y_e$) that represents the trajectory which a massive stars central region takes after its silicon core burns. Our computed mass fractions were found in decent comparison in most cases, and up to a factor 4 difference was noted when compared with the Independent Particle Model results. The weak interaction (ec and bd) rates were calculated in a totally microscopic fashion using the proton neutron quasiparticle random phase ap proximation model and without assuming the Brink Axel hypothesis. The rates were computed for a wide range of density ($10$-$10^{11}$) g/cm$^3$ and temperature (0.01-30) GK. In comparison with large scale shell model, our computed rates were found bigger at high values of core temperature. The current study may contribute in a more realistic simu lation of stellar evolution processes and modeling of core collapse supernovae.
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