标题： 恒星弱相互作用速率的估计值，适用于质量数A=65-80范围内的核素 显示英文标题

标题： Estimates of Stellar Weak Interaction Rates for Nuclei in the Mass Range A=65-80

摘要： 我们估算质量数A=65-80的核素的轻子捕获和发射率，以及中微子能量损失率。 这些率是在适合广泛天体物理应用的温度/密度网格上计算的，包括晚期恒星演化和X射线爆发的模拟。 我们单粒子和经验启发模型的基本输入包括i) 实验测得的能级和弱衰变信息，ii) 基于实验观察到的允许跃迁系统性的对实验未测量跃迁的矩阵元估计，以及iii) 由fp壳层的壳模型计算以及(n,p)和(p,n)实验所激发的GT共振中心的估计。 涉及费米共振（同位素类似态）的跃迁也包括在内，并且对于许多感兴趣的质子丰富的核素，这些跃迁主导了速率，这些核素的实验确定的基态寿命尚不可用。 为了将我们的结果与更详细的基于壳模型的计算进行比较，我们也计算了质量数A=60-65范围内核素的弱率，Langanke和Martinez-Pinedo已为此提供了速率。 对于这些约30个核素，电子捕获和B-衰变率在适用于超新星前恒星演化的广泛温度和密度范围内的典型偏差小于两倍或三倍。 我们还讨论了与恒星弱率计算中使用的分区函数相关的一些细节，并表明正确处理分区函数对于估计高温β衰变率至关重要。 基于未收敛的Lanczos计算的分区函数可能导致高温β衰变率的估计值系统性偏低。 显示英文摘要

摘要： We estimate lepton capture and emission rates, as well as neutrino energy loss rates, for nuclei in the mass range A=65-80. These rates are calculated on a temperature/density grid appropriate for a wide range of astrophysical applications including simulations of late time stellar evolution and x-ray bursts. The basic inputs in our single particle and empirically inspired model are i) experimentally measured level and weak decay information, ii) estimates of matrix elements for allowed experimentally-unmeasured transitions based on the systematics of experimentally observed allowed transitions, and iii) estimates of the centroids of the GT resonances motivated by shell model calculations in the fp shell as well as by (n,p) and (p,n) experiments. Transitions involving Fermi resonances (isobaric analog states) are also included and dominate the rates for many interesting proton rich nuclei for which an experimentally-determined ground state lifetime is unavailable. To compare our results with more detailed shell model based calculations we also calculate weak rates for nuclei in the mass range A=60-65 for which Langanke and Martinez-Pinedo have provided rates. The typical deviation in the electron capture and B- decay rates for these ~30 nuclei is less than a factor of two or three for a wide range of temperature and density appropriate for pre-supernova stellar evolution. We also discuss some subtleties associated with the partition functions used in calculations of stellar weak rates and show that the proper treatment of the partition functions is essential for estimating high temperature beta decay rates. Partition functions based on un-converged Lanczos calculations can result in estimates of high temperature beta decay rates that are systematically low.