与核心坍缩超新星核合成有关的$^{13}$ N（PDMATHAAB，$p$）$^{16}$ O反应的首次直接测量
First direct measurement of the $^{13}$N($α$,$p$)$^{16}$O reaction relevant for core-collapse supernovae nucleosynthesis
摘要：
了解核心坍缩超新星（CCSN）的爆炸机制对于使用模型观测比较准确地模拟不同祖星的CCSN场景非常重要。各种核反应速率的不确定性相关的CCSN方案强烈影响这些恒星模型的准确性。在这些反应中，已发现$^{13}$ N（$α$，$p$）$^{16}$ O反应在不同温度下影响CCSN的各个阶段。这项工作提出了第一次直接测量的$^{13}$ N（$α$，$p$）$^{16}$ O反应进行使用34.6 MeV的放射性$^{13}$ N离子束和主动靶探测器MUSIC（多采样电离室）在阿贡国家实验室。由此产生的总$^{13}$ N（$α$，$p$）$^{16}$ O反应截面从这个测量的质心能量范围为3.26 - 6.02 MeV的，并与计算使用豪泽-Feshbach形式主义。在CCSN温度下，反应速率的不稳定性显著降低。
英文摘要：
Understanding the explosion mechanism of a core-collapse supernova (CCSN) is important to accurately model CCSN scenarios for different progenitor stars using model-observation comparisons. The uncertainties of various nuclear reaction rates relevant for CCSN scenarios strongly affect the accuracy of these stellar models. Out of these reactions, the $^{13}$N($α$,$p$)$^{16}$O reaction has been found to affect various stages of a CCSN at varying temperatures. This work presents the first direct measurement of the $^{13}$N($α$,$p$)$^{16}$O reaction performed using a 34.6 MeV beam of radioactive $^{13}$N ions and the active-target detector MUSIC (MUlti-Sampling Ionization Chamber) at Argonne National Laboratory. The resulting total $^{13}$N($α$,$p$)$^{16}$O reaction cross sections from this measurement in the center-of-mass energy range of 3.26 - 6.02 MeV are presented and compared with calculations using the Hauser-Feshbach formalism. Uncertainties in the reaction rate have been dramatically reduced at CCSN temperatures.
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