论文标题
从中子恒星合并弹出的R过程的剥离
Spallation of r-Process Nuclei Ejected from a Neutron Star Merger
论文作者
论文摘要
中子星星合并（NSM）是快速中子捕获（R-Process）核合成位点，它们以高速度从0.1C驱射到高达0.6C。因此，从NSM事件中弹出的R-Process核具有足够的能量，可以引发与星际介质（ISM）颗粒的剥落反应。借助ISM中高速重核传播的厚目标模型，我们发现散布反应可能会将R过程的丰度模式转移到太阳数据上，尤其是在附近核的R-Process峰的低质量边缘附近，而附近核的核心具有非常不同的丰度。散布效应既取决于核合成计算和传播过程的R过程和核物理学输入的天体物理条件。这项工作扩展了[Wang等人（2019年）]，通过关注核物理学对剥落效应的影响。
Neutron star mergers (NSMs) are rapid neutron capture (r-process) nucleosynthesis sites, which eject materials at high velocities, from 0.1c to as high as 0.6c. Thus the r-process nuclei ejected from a NSM event are sufficiently energetic to initiate spallation reactions with the interstellar medium (ISM) particles. With a thick-target model for the propagation of high-speed heavy nuclei in the ISM, we find that spallation reactions may shift the r-process abundance patterns towards solar data, particularly around the low-mass edges of the r-process peaks where neighboring nuclei have very different abundances. The spallation effects depend both on the astrophysical conditions of the r-process nuclei and nuclear physics inputs for the nucleosynthesis calculations and the propagation process. This work extends that of [Wang et al.(2019)] by focusing on the influence of nuclear physics variations on spallation effects.
