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- W3104144251 abstract "Abstract The chemical abundances of the metal-poor stars in the stellar stream provide important information for setting constraints on models of neutron-capture processes. The study of these stars could gives us a better understanding of the r -process nucleosynthesis and chemical composition of the early Galaxy. Using the updated main r -process and weak r -process patterns, we fit abundances in the stellar stream stars. The weak r -process component coefficients are almost constant for the sample stars, including r -rich stars, which means that both the weak r -process and Fe are produced as primary elements from Type II supernovae and their yields have nearly a constant mass fraction. The difference between the stream stars and r -rich stars is obvious. For the stream stars, the fact that the increased trend in the main r -process component coefficients as metallicity increases means a gradual increase in the production of main r -process elements relative to iron. This behaviour implies that the masses of progenitors for the main r -process are smaller than those of the weak r -process. Furthermore, we find that the metal-poor stream star HD 237846 is a weak r -process star." @default.
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- W3104144251 date "2013-01-01" @default.
- W3104144251 modified "2023-09-24" @default.
- W3104144251 title "Study of the Abundance Patterns in the Metal-Poor Stellar Stream" @default.
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- W3104144251 doi "https://doi.org/10.1017/pasa.2012.015" @default.
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