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首页> 外文期刊>Physica Scripta: An International Journal for Experimental and Theoretical Physics >Nuclear inputs of key iron isotopes for core-collapse modeling and simulation
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Nuclear inputs of key iron isotopes for core-collapse modeling and simulation

机译：关键铁同位素的核输入，用于核塌陷建模和模拟

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摘要

From the modeling and simulation results of presupernova evolution of massive stars, it was found that isotopes of iron, ~(54–56)Fe, play a significant role inside the stellar cores, primarily decreasing the electron-to-baryon ratio (Y_e) mainly via electron capture processes thereby reducing the pressure support. The neutrinos produced as a result of these capture processes are transparent to the stellar matter and assist in cooling the core, thereby reducing the entropy. The structure of the presupernova star is altered both by the changes in Y_e and the entropy of the core material. Here we present the microscopic calculation of Gamow–Teller strength distributions for isotopes of iron. The calculation is also compared with other theoretical models and experimental data. Presented also are stellar electron capture rates and associated neutrino cooling rates, due to isotopes of iron, in a form suitable for simulation and modeling codes. It is hoped that the nuclear inputs presented here should assist core-collapse simulators in the process of fine-tuning of the Y_e parameter during various phases of presupernova evolution of massive stars. A reliable and accurate time evolution of this parameter is a possible key to generate a successful explosion in modeling of core-collapse supernovae.
机译：根据大质量恒星超新星演化的建模和模拟结果，发现〜（54-56）Fe的铁同位素在恒星核内部起着重要作用，主要是降低了电子与重子的比值（Y_e）主要通过电子捕获过程，从而降低压力支持。这些捕获过程产生的中微子对恒星物质是透明的，并有助于冷却核，从而降低熵。超新星前的恒星的结构通过Y_e的变化和核心材料的熵而改变。在这里，我们介绍铁同位素的Gamow-Teller强度分布的微观计算。该计算也与其他理论模型和实验数据进行了比较。还介绍了由于铁的同位素引起的恒星电子捕获速率和相关的中微子冷却速率，其形式适合于模拟和建模代码。希望这里介绍的核输入在大质量恒星超新星前演化的各个阶段中，可以帮助核塌陷模拟器对Y_e参数进行微调。该参数可靠且准确的时间演化是在核心塌陷超新星建模中成功产生爆炸的可能关键。

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