The Yields of r-Process Elements and Chemical Evolution of the Galaxy |
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| Authors: | Zhe Chen Jiang Zhang YanPing Chen WenYuan Cui Bo Zhang |
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| Institution: | (1) Department of Physics, Hebei Normal University, Shijiazhuang, 050016, P.R. China;(2) Shijiazhuang Foreign Language School, 050000 Shijiazhuang, P.R. China;(3) Department of Physics, Hebei Normal University, Shijiazhuang, 050016, P.R. China;(4) Shijiazhuang University of Economics, Shijiazhuang, 050031, P.R. China;(5) Department of Physics, Hebei Normal University, Shijiazhuang, 050016, P.R. China |
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| Abstract: | The supernova yields of r-process elements are obtained as a function of the mass of their progenitor stars from the abundance patterns of extremely metal-poor stars on the left-side {Ba/Mg}]--{Mg/H}] boundary with a procedure proposed by Tsujimoto and Shigeyama. The ejected masses of r-process elements associated with stars of progenitor mass M
ms ≤ 18 M
⊙ are infertile sources and the SNe II with 20 M
⊙ ≤ M
ms ≤ 40 M
⊙ are the dominant source of r-process nucleosynthesis in the Galaxy. The ratio of these stars 20 M
⊙ ≤ M
ms ≤ 40 M
⊙
with compared to the all massive stars is about∼ 18%. In this paper, we present a simple model that describes a star's r/Fe] in terms of the nucleosynthesis yields of r-process elements and the number of SN II explosions. Combined the r-process yields obtained by our procedure with the scatter model of the Galactic halo, the observed abundance patterns of the metal-poor stars can be well reproduced. |
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| Keywords: | Element abundance Chemical evolution The yield of r-process element |
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