Production of ^(22)Na Secondary Beam  

作　　者：JIANG Chao LIAN Gang WANG Bao-xiang SU Jun BAI Xi-xiang ZENG Sheng ZHENG Yong-nan ZHU Sheng-yun Zhu Li-hua LIU Wei-ping LI Zhi-hong WANG You-bao GUO Bing QIN Xing LI Yun-ju 

机构地区：[1]不详 [2]Institute of Modern Physics, Shanxi Normal University, Linfen 041004, China [3]Institute of Physical Engineering, Zhengzhou University, Zhengzhou 450052, China

出　　处：《Annual Report of China Institute of Atomic Energy》2007年第1期114-115,共2页中国原子能科学研究院年报（英文版）

基　　金：National Science Foundation of China (0575136);National Natural Science Foundation of China (10605039)

摘　　要：^22Na is an important radioactive nuclide involved in the explosive hydrogen burning process in stars, and is also the oftenest used β^＋-source in positron-annihilation spectroscopy. Its half-life is 2.6 a and is produced in novae （Clayton 1975）.The study of the isotopic composition of meteorites has revealed some perplexing anomalies, in that the isotopic abundances of certain elements do not agree with the abundances of terrestrial material. Such anomalies include the presence of excess ^129Xe, thought to be due to the decay of ^129I, excess ^26Mg, the daughter of ^26Al, and the presence of almost pure ^22Na, known as Na-E.22Na is an important radioactive nuclide involved in the explosive hydrogen burning process in stars, and is also the oftenest used β+-source in positron-annihilation spectroscopy. Its half-life is 2.6 a and

关 键 词：天体物理学 钠 氢燃烧过程 放射性核素 

分 类 号：P14[天文地球—天体物理]