论文标题
流行III超新星弹出的结构会影响极度金属贫困星的元素丰度吗？
Does the structure of Pop III supernova ejecta affect the elemental abundance of extremely metal-poor stars?
论文作者
论文摘要
第一代无金属（POP III）恒星对于最早的结构形成阶段的重元素至关重要。它们的质量尺度可以源自极为金属贫困（EMP）星的元素丰度模式，这些恒星被认为继承了均匀混合的超新星（SN）弹出的丰度。如果扩展的弹出保持其初始分层结构，则EMP恒星的元素丰度模式可能与均匀的喷射恒星不同。在这项工作中，我们对正常核心散射SNE（CCSNE）的金属富集进行数值模拟，其祖细胞质量为$ 25 \ {\ rm M} _ {\ bigodot} $和爆炸能量0.77---10 b（$ 1 \ \ \ \ rm B} = 10^10^51}我们发现，在所有型号中，SN壳落入了中央Minihalo。在回想起的云中，对于分层弹出的丰度$ {\ rm [m/fe]} $与均匀的弹出仅在$ \ pm \ pm 0.4 $ 0.4 $ dex的范围内不同。只有包含CA或较轻元素的外层到达光环，其中$ {\ rm [c/fe]} = 1.49 $。这意味着即使平均丰度比$ {\ rm [c/fe]} = -0.65 $，CCSN也可以从CCSN形成C-增强的金属贫困（CEMP）恒星。
The first generation of metal-free (Pop III) stars are crucial for the production of heavy elements in the earliest phase of structure formation. Their mass scale can be derived from the elemental abundance pattern of extremely metal-poor (EMP) stars, which are assumed to inherit the abundances of uniformly mixed supernova (SN) ejecta. If the expanding ejecta maintains its initial stratified structure, the elemental abundance pattern of EMP stars might be different from that from uniform ejecta. In this work we perform numerical simulations of the metal enrichment from stratified ejecta for normal core-collapse SNe (CCSNe) with a progenitor mass $25 \ {\rm M}_{\bigodot}$ and explosion energies 0.7--10 B ($1 \ {\rm B} = 10^{51}$ erg). We find that SN shells fall back into the central minihalo in all models. In the recollapsing clouds, the abundance ratio ${\rm [M/Fe]}$ for stratified ejecta is different from the one for uniform ejecta only within $\pm 0.4$ dex for any element M. We also find that, for the largest explosion energy (10 B), a neighboring halo is also enriched. Only the outer layers containing Ca or lighter elements reach the halo, where ${\rm [C/Fe]} = 1.49$. This means that C-enhanced metal-poor (CEMP) stars can form from the CCSN even with an average abundance ratio ${\rm [C/Fe]} = -0.65$.
