爆炸恒星温度下类恒星中子场的产生
Production of Quasi-Stellar Neutron Field at Explosive Stellar Temperatures
摘要：
中子引起的不稳定同位素反应在天体物理学情景中发生的核合成$i$ -、$r$-、$p$-、$rp$ -和$νp$ -过程中发挥关键作用。虽然使用中子飞行时间方法可以直接测量长寿命不稳定同位素的截面，但目前可用的中子强度（$\approx10^{6}$ n/s）需要大样本，这对于寿命较短的同位素是不可行的。在过去的40年里，$^{7}$ Li $(p,n)$反应已经被用来在$\approx$ 0.3 GK的恒星温度下提供具有显著更高强度的中子场，使得沿着$s$ -过程路径的许多横截面的成功测量成为可能。在本文中，我们描述了一种新的方法，使用该反应在$\approx$ 1.5-3.5 GK的温度下产生中子场，与对流壳层C/Ne燃烧、爆炸性Ne/C燃烧和核心坍缩超新星等情景有关。这种方法将允许在爆炸温度下直接测量许多重要反应的截面，例如$^{26}$ Al $(n,p)$、$^{75}$ Se $(n,p)$和$^{56}$ Ni $(n,p)$。
英文摘要：
Neutron-induced reactions on unstable isotopes play a key role in the nucleosynthesis $i$--, $r$--, $p$--, $rp$-- and $νp$--processes occurring in astrophysical scenarios. While direct cross section measurements are possible for long-living unstable isotopes using the neutron Time-of-Flight method, the currently available neutron intensities ($\approx10^{6}$ n/s) require large samples which are not feasible for shorter lifetime isotopes. For the last four decades, the $^{7}$Li$(p,n)$ reaction has been used to provide a neutron field at a stellar temperature of $\approx$ 0.3 GK with significantly higher intensity, allowing the successful measurement of many cross sections along the $s$-process path. In this paper we describe a novel method to use this reaction to produce neutron fields at temperatures of $\approx$ 1.5-3.5 GK, relevant to scenarios such as convective shell C/Ne burning, explosive Ne/C burning, and core-collapse supernovae. This method will allow direct cross section measurements of many important reactions at explosive temperatures, such as $^{26}$Al$(n,p)$, $^{75}$Se$(n,p)$ and $^{56}$Ni$(n,p)$.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
