KEK Isotope Separation System (KISS)
KEK Isotope Separation System (KISS)
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KEK 同位素分离系统 (KISS)
DOI：
10.1080/10619127.2018.1529984
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发表时间：
2018
影响因子：
--
通讯作者：
H. Miyatake
中科院分区：
文献类型：
--
作者：
Y. Watanabe;Y. Hirayama;H. Miyatake
金和铂等重元素在我们的宇宙中是在哪里以及如何合成的？这是核物理学的原始问题之一，KEK 同位素分离系统 (KISS) 的构建就是为了尝试回答这个问题。 Burbidge、Burbidge、Fowler 和 Hoyle 于 1957 年提出通过九个天体物理过程合成恒星中的元素[1]。在这些过程中，快速中子俘获过程（r过程）被认为是比铁重的元素丰度的一半造成的。它发生在高中子密度和高温的环境下。 r过程的天体物理地点有几个候选地点，例如II型超新星和双中子星合并。最近对双中子星合并产生的引力波和电磁辐射的首次观测[2]使此类合并成为热门话题，因为它们被认为是 r 过程天体物理地点的有希望的候选者。尽管人们在实验和理论研究上投入了大量精力来确定天体物理环境，但迄今为止，r过程的天体物理地点仍然是个谜。部分原因是缺乏许多原子核属性的信息，例如寿命和质量，这些在 r 过程中起着至关重要的作用。最重要的原子核是中子幻数 50、82 和 126 附近不稳定的富中子原子核。r 过程在高中子密度环境下经过极其富中子的原子核。中子幻数增强的中子分离能导致沿路径出现等待点，并且等待点核被认为是观测到的 r 过程对太阳丰度分布贡献的峰值的起源。特别是，金和铂是 A= 195 附近太阳丰度分布峰值的一部分，据推测源自中子幻数为 126 的 r 过程等待核。由于难以通过裂变、聚变和碎裂等传统核生产方法生产这些核，因此这些核的核特性尚未在很大程度上进行实验研究。这些同位素也很难在现有的在线同位素分离器 (ISOL) 设施中提取，因为它们是难熔元素。KISS 项目于 2011 年启动，旨在生产这些难熔元素，提取它们，并探索它们的核特性，以确定 r 过程的天体物理环境。该项目是在粒子与核研究所 (IPNS)、高能加速器研究组织 (KEK) 和 RIKEN Nishina 加速器科学中心的合作下执行的。 2015 年 4 月，为了推进 KISS 项目，在 RIKEN IPNS 下成立了和光核科学中心。
Where and how are the heavy elements such as gold and platinum synthesized in our universe? It is one of nuclear physics’ original questions, which the KEK Isotope Separation System (KISS) was constructed to attempt to answer. Burbidge, Burbidge, Fowler, and Hoyle proposed the synthesis of the elements in stars via nine astrophysical processes in 1957 [1]. Among those processes, the rapid neutron capture process (r-process) is considered to be responsible for half of the abundance of the elements heavier than iron. It occurs under an environment with a high neutron density and a high temperature. There are several candidates for the astrophysical site of the r-process, such as type-II supernovae and binary neutron star mergers. The recent first observation of gravitational waves and electromagnetic radiation from a binary neutron star merger [2] makes such mergers a hot topic now that they are considered a promising candidate for the astrophysical site of the r-process. Although energetic efforts have been poured into experimental and theoretical research to determine the astrophysical environment, so far, the astrophysical site for the r-process remains a mystery. It is partially because of a lack of information for properties of many nuclei, such as a lifetime and a mass, which have crucial roles in the r-process. The most crucially important nuclei are unstable, neutron-rich nuclei around neutron magic numbers 50, 82, and 126. The r-process goes through extremely neutron-rich nuclei under a high neutron density environment. The enhanced neutron separation energy of neutron magic numbers results in waiting points along the path, and the waiting point nuclei are considered to be origins for peaks in the observed r-process contribution to the solar abundance distribution. Particularly, gold and platinum are part of a peak in the solar abundance distribution near A= 195, which is presumed to originate from r-process waiting nuclei with the neutron magic number 126. The nuclear properties of these nuclei as yet remain largely unstudied experimentally due to the difficulty in producing them by traditional nuclear production methods such as fission, fusion, and fragmentation. Those isotopes are also difficult to extract in existing Isotope Separator On-Line (ISOL) facilities, because they are refractory elements.The KISS project was launched in 2011 to produce these refractory elements, extract them, and explore their nuclear properties for determination of the astrophysical environment of the r-process. The project is executed under a collaboration between the Institute of Particle and Nuclear Studies (IPNS), High Energy Accelerator Research Organization (KEK), and RIKEN Nishina Center for Accelerator-Based Science. Wako Nuclear Science Center was founded under IPNS at RIKEN to promote the KISS project in April 2015.
用于在线同位素分离器的激光离子源
DOI：
10.1016/s0168-583x(96)01017-8
发表时间：
1997
期刊：
影响因子：
--
作者：
P. Duppen
通讯作者：
P. Duppen
影响因子：
8.6
作者：
C. Dasso;G. Pollarolo;A. Winther
通讯作者：
C. Dasso;G. Pollarolo;A. Winther
奇异的原子核和原子质量
DOI：
10.1007/978-3-642-55560-2
发表时间：
2003
期刊：
--
影响因子：
--
作者：
J. Äystö;P. Dendooven;A. Jokinen;M. Leino
通讯作者：
M. Leino