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Historically, the weak s-process contribution to metal-poor stars is thoughtto be extremely small, due to the effect of the secondary-like nature of theneutron source 22Ne(a;n)25Mg in massive stars, which means that metal-poor weaks-process stars could not be found. ET0097 is the first observedcarbon-enhanced metal-poor (CEMP) star in the Sculptor dwarf spheroidal galaxy.Because C is enriched and the elements heavier than Ba are not overabundant,ET0097 can be classified as a CEMP-no star. However, this star showsoverabundances of lighter n-capture elements (i.e., Sr, Y and Zr). In thiswork, having adopted the abundance decomposition approach, we investigate theastrophysical origins of the elements in ET0097. We find that the lightelements and iron-peak elements (from O to Zn) of the star mainly originatefrom the primary process of massive stars and the heavier n-capture elements(heavier than Ba) mainly come from the main r-process. However, the lightern-capture elements such as Sr, Y and Zr should mainly come from the primaryweak s-process. The contributed fractions of the primary weak s-process to theSr, Y and Zr abundances of ET0097 are about 82%, 84% and 58% respectively,suggesting that the CEMP star ET0097 should have the footprints of the weaks-process. The derived result should be a significant evidence that the weaks-process elements can be produced in metal-poor massive stars.

Footprints of the weak s-process in the carbon-enhanced metal-poor star ET0097