Abundance Distribution of Slow-Process Main Heavy Elements in AGB Stars
ZHANG Miao-Jing1,2,3, ZHANG Bo1,3,4, LI Guang-Lie1,3
1Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100039
2Department of Physics and Electronic Science, Guangxi Normal University, Guilin 541004
3Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator of Lanzhou, Lanzhou 730000
4Department of Physics, Hebei Normal University, Shijiazhuang 050016
Abundance Distribution of Slow-Process Main Heavy Elements in AGB Stars
1Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100039
2Department of Physics and Electronic Science, Guangxi Normal University, Guilin 541004
3Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator of Lanzhou, Lanzhou 730000
4Department of Physics, Hebei Normal University, Shijiazhuang 050016
Abstract： By re-analysing the results of the theoretical abundance of asymptotic giant branch (AGB) stellar models and the observed abundances of 51 AGB samples, we find that the abundance distribution of s-process main heavy (SMH) elements of any AGB star is similar to the scaled s-process main component of the solar system. This means that superposition of the SMH element abundance distributions of AGB stars should be similar to the scaled solar s-process main component. As a conclusion, the abundance pattern of the solar SMH elements is not only an average result of a complex chemical evolution of galaxy, but also a typical one that can be used as a standard in abundance investigation.
ZHANG Miao-Jing;;ZHANG Bo;;LI Guang-Lie;. Abundance Distribution of Slow-Process Main Heavy Elements in AGB Stars[J]. 中国物理快报, 2003, 20(6): 962-964.
ZHANG Miao-Jing, , ZHANG Bo, , LI Guang-Lie,. Abundance Distribution of Slow-Process Main Heavy Elements in AGB Stars. Chin. Phys. Lett., 2003, 20(6): 962-964.
2003, Vol. 20 
