标题： 极金属缺乏星中第一代超新星喷发遗迹的化石印记 显示英文标题

标题： Fossil Imprints of the First Generation Supernova Ejecta in Extremely Metal-Deficient Stars

摘要： 利用不同前身星质量的理论核心坍缩超新星模型的核合成计算结果表明，极度金属缺乏星（[Fe/H] < -2.5）中观测到的C、Mg、Si、Ca和H的丰度分布模式与第一代超新星遗迹（SNRs）中观测到的分布模式一致。这表明大多数[Fe/H] < -2.5的恒星是由单个超新星（SN）事件形成的。 为了获得重元素与氢的比例，推导出一个公式来估算当超新星遗迹（SNR）发生在具有原始丰度的星际物质中时，被扫过的氢的质量。 我们使用[Mg/H]来表示金属丰度，而不是[Fe/H]。 这些SNRs预测的金属丰度[Mg/H]范围从约-4到约-1.5，且超新星中Mg的质量与其前身星的质量有很好的相关性。 因此，极度金属缺乏星中的观测[Mg/H]与前身星的质量相对应。 较大的[Mg/H]对应于较大的前身星质量。 因此，所谓的“年龄-金属丰度关系”不适用于[Fe/H] < -2.5的恒星。 相比之下，理论上SNRs中的[Mg/Fe]比值趋势与极度金属缺乏星中的不同。 还显示了[Mg/Fe]的观测趋势可以预测每个SN的Fe产额，前提是[Mg/H]与前身星质量之间的对应关系已知。 由此得到的Fe产额与来自超新星光变曲线分析得出的结果一致。 这表明在超新星爆炸开始或质量截断建模方面仍然存在问题。 显示英文摘要

摘要： Using results of nucleosynthesis calculations for theoretical core-collapse supernova models with various progenitor's masses, it is shown that abundance patterns of C, Mg, Si, Ca, and H seen in extremely metal-deficient stars with [Fe/H] < -2.5 follow those seen in the individual first generation supernova remnants (SNRs). This suggests that most of the stars with [Fe/H] < -2.5 were made from individual supernova (SN) events. To obtain the ratio of heavy elements to hydrogen, a formula is derived to estimate the mass of hydrogen swept up by a SNR when it occurs in the interstellar matter with the primordial abundances. We use [Mg/H] to indicate the metallicities instead of [Fe/H]. The metallicities [Mg/H] predicted from these SNRs range from ~-4 to ~-1.5 and the mass of Mg in a SN is well correlated with its progenitor's mass. Thus the observed [Mg/H] in an extremely metal deficient star has a correspondence to the progenitor's mass. A larger [Mg/H] corresponds to a larger progenitor's mass. Therefore, so called `age-metallicity relation' does not hold for stars with [Fe/H] < -2.5. In contrast, the [Mg/Fe] ratios in the theoretical SNRs have a different trend from those in extremely metal-deficient stars. It is also shown that the observed trend of [Mg/Fe] can predict the Fe yield of each SN given the correspondence of [Mg/H] to the progenitor's mass. The Fe yields thus obtained are consistent with those derived from SN light curve analyses. This indicates that there is still a problem in modelling a core-collapse supernova at its beginning of explosion or mass cut.