| Original Articles |
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R-Process Nucleosynthesis and Galactic Chemical Evolution of
the Ba Peak Elements |
| SONG Han-Feng1;ZHANG Bo1,2;ZHANG Jiang1;WU Hai-Bin1,4;PENG Qiu-He3 |
| 1Department of Physics, Hebei Normal University, Shijiazhuang 050016
2Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator, Lanzhou 730000
3Department of Astronomy, Nanjing University, Nanjing 210093
4Institute of Physics, Shijiazhuang Teachers college, Shijiazhang 050081 |
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| Cite this article: |
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SONG Han-Feng, ZHANG Bo, ZHANG Jiang et al 2003 Chin. Phys. Lett. 20 2084-2087 |
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Abstract Nucleosynthesis yield is a very important parameter of the Galactic chemical evolution model. We adopt the same method of Tsujimoto to derive the r-process yields of various mass SNe II at low metallicities from the new observed [Ba/Fe]-[Fe/H] trend. %but we get rid of the stars such as CS22892-052, CS31082. Furthermore, we present a new formula of r-process nucleosynthesis yields. We also consider the various neutron sources and set up four cases, namely A, B, C and D to calculate the abundance evolution of Ba peak elements in the solar neighborhood. Our results show that the r-process could be associated with a secondary event in massive stars (i.e., 18M < M < 50). Therefore, the r-process could be associated with a secondary event in massive stars. Both the neutron source and the seed nuclei must be freshly manufactured by the stars instead of depending upon the initialmetallicity abundance.
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| Keywords:
97.10.Cv
98.35.Bd
97.10.Tk
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Published: 01 November 2003
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| PACS: |
97.10.Cv
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(Stellar structure, interiors, evolution, nucleosynthesis, ages)
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98.35.Bd
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(Chemical composition and chemical evolution)
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97.10.Tk
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(Abundances, chemical composition)
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