论文标题
$^{13} $ n（$α$，$ p $）$^{16} $的第一个直接测量
First direct measurement of the $^{13}$N($α$,$p$)$^{16}$O reaction relevant for core-collapse supernovae nucleosynthesis
论文作者
论文摘要
了解使用模型观察性比较来准确地对不同祖细胞的CCSN场景进行准确对CCSN场景进行对CCSN场景进行对CCSN场景进行建模很重要的爆炸机制。与CCSN场景相关的各种核反应速率的不确定性强烈影响这些恒星模型的准确性。在这些反应中，发现$^{13} $ n（$α$，$ p $）$^{16} $ o反应会影响不同温度下的CCSN的各个阶段。这项工作介绍了$^{13} $ n（$α$，$ p $）$^{16} $ o的第一个直接测量，该反应使用34.6 meV的放射性$^{13} $ n离子和Agronne National实验室的Active-Actiact-Artip-artarget检测器音乐（多样化的电离电离室）进行。由此产生的总$^{13} $ n（$α$，$ p $）$^{16} $ o反应横截面的质量中心能量范围为3.26-6.02 meV，并与使用Hauser-feshbach形式主义的计算进行了比较。在CCSN温度下，反应速率的不确定性已大大降低。
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.
