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首页> 外文期刊>Physica Scripta: An International Journal for Experimental and Theoretical Physics >Temperature-dependent nuclear partition functions and abundances in the stellar interior
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Temperature-dependent nuclear partition functions and abundances in the stellar interior

机译：恒星内部的温度依赖性核分配功能和丰度

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摘要

We calculate the temperature-dependent nuclear partition functions (TDNPFs) and nuclear abundances for 728 nuclei, assuming nuclear statistical equilibrium (NSE). The theories of stellar evolution support NSE. Discrete nuclear energy levels have been calculated microscopically, using the pn-QRPA theory, up to an excitation energy of 10 MeV in the calculation of the TDNPFs. This feature of our paper distinguishes it from previous calculations. Experimental data is also incorporated wherever available to ensure the reliability of our results. Beyond 10 MeV, we employ a simple Fermi gas model and perform integration over the nuclear level densities to approximate the TDNPFs. We calculate nuclidic abundances, using the Saha equation, as a function of three parameters: stellar density, stellar temperature and the lepton-to-baryon content of stellar matter. All these physical parameters are considered to be extremely important in the stellar interior. The results obtained in this paper show that the equilibrium configuration of nuclei remains unaltered by increasing the stellar density (only the calculated nuclear abundances increase by roughly the same order of magnitude). Increasing the stellar temperature smoothes the equilibrium configuration showing peaks at the neutron-number magic nuclei.
机译：假设核统计平衡（NSE），我们计算728个核的温度依赖性核分配函数（TDNPFs）和核丰度。恒星演化理论支持NSE。在计算TDNPF时，已使用pn-QRPA理论以微观方式计算了离散核能级，直到10 MeV的激发能。本文的此功能将其与以前的计算区分开。只要有可用的地方，实验数据也会被合并，以确保我们结果的可靠性。超过10 MeV，我们采用简单的费米气体模型，并在核能级密度上进行积分以近似TDNPF。我们使用Saha方程，根据三个参数来计算核素丰度：恒星密度，恒星温度和恒星物质的轻子至重子含量。所有这些物理参数都被认为在恒星内部极为重要。本文获得的结果表明，通过增加恒星密度，原子核的平衡构型保持不变（仅计算出的核丰度增加了大致相同的数量级）。恒星温度的升高使平衡构型变得平滑，平衡构型在中子数魔核处出现峰值。

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