Spectroscopic Factors for Low-lying 16N Levels and Astrophysical 15N（n, γ）16N Reaction Rate  

作　　者：WU Zhi-dan GUO Bing LI Zhi-hong LI Yun-ju SU Jun PAN Dan-yang YAN Sheng-quan LI Er-tao BAI Xi-xiang DU Xian-chao FAN Qi-wen GAN Lin HE Jian-jun JIN Sun-jun JING Long LI Long LI Zhi-chang LIAN Gang LIU Jian-cheng SHEN Yang-ping WANGYou-bao YU Xiang-qing ZENG Sheng ZHANG Li-yong ZHANG Wei-jie LIU Wei-ping 

机构地区：[1]Depar tment ofNuclear Physics [2]School of Physics and Nuclear Energy Engineer ing, Beihang University [3]CollegeofPhysics Science and Technology, Shenzhen University [4]Institute of Modern Physics, Chinese Academy of Sciences

出　　处：《Annual Report of China Institute of Atomic Energy》2013年第1期47-47,共1页中国原子能科学研究院年报（英文版）

基　　金：Supported by National Natural Science Foundation of China(11075219,11321064,11375269,11275272,1275018);973 Program of China(2013CB834406)

摘　　要：Fluorine is a key element for nucleosynthetic studies since it is extremely sensitive to the physical conditions within stars.The astrophysical site to produce fluorine is suggested to be asymptotic giant branch stars.In these stars the 15N(n,γ)16N reaction could affect the abundance of fluorine by competing with 15N(α,γ)19F.In the present work,the angular distribution of the 15N(7Li,6Li)16N reaction

关 键 词：LYING competing EXTREMELY stars branch ASYMPTOTIC FLUORINE ABUNDANCE angular giant 

分 类 号：P148[天文地球—天体物理]