论文标题
R过程的辐射性中子捕获反应速率
Radiative neutron capture reaction rates for r-process nucleosynthesis
论文作者
论文摘要
通过快速中子捕获过程（R-process），大约一半的铁元素在恒星中合成。恒星环境在短时间内提供了很高的中子通量（$ \ sim $秒），这有利于创建逐渐富含中子的核，直到达到等待点，此后不进行进一步的中子捕获反应。在这一点上，这种极其富含中子的核通过$β^ - $衰减变得稳定。对R过程的详细理解仍然是虚幻的。在目前的工作中，我们探索了辐射性中子捕获（N，$γ$）的横截面，以及在R-Process峰附近质量为80的RAPROCESS峰附近的反应速率。在某些情况下，固有的不确定性仍然很大，尤其是在中子富含核的情况下。当存在低能增强时，它会导致中子捕获的反应率显着增加。
About half of the elements beyond iron are synthesized in stars by rapid-neutron capture process (r-process). The stellar environment provides very high neutron flux in a short time ($\sim$ seconds) which is conducive for the creation of progressively neutron-rich nuclei till the waiting point is reached after which no further neutron capture reactions proceed. At this point such extremely neutron-rich nuclei become stable via $β^-$ decay. A detailed understanding of the r-process remains illusive. In the present work, we explore the radiative neutron-capture (n,$γ$) cross sections and reaction rates around the r-process peak near mass number eighty. The inherent uncertainties remain large in some cases, particularly in case of neutron-rich nuclei. When the low-energy enhancement exists, it results in significant increase in the reaction rate for neutron-capture.
