QED V：星系风中金属载荷随元素核合成起源的变化
QED V: Variations in metal loading of galactic winds with element nucleosynthetic origin
AI总结：
通过高分辨率模拟，研究不同核合成来源（Ia型超新星、II型超新星和AGB星）产生的金属在星系风中的载荷差异，发现约0.3 dex的变化，称为差异金属载荷，并质疑基于丰度诊断的星系形成解释。
摘要：
Ia型超新星、II型超新星和渐近巨星分支（AGB）星是恒星核合成的重要场所，但它们在爆发率、星系内位置以及喷出物的平均热能和丰度分布方面存在巨大差异。在本系列的前期论文中，我们已经表明，由II型超新星新合成的金属中有很大一部分会迅速通过星系风流失——即星系风具有金属载荷。本文研究由Ia型超新星和AGB星返回的元素是否也具有类似的金属载荷，或者金属载荷是否随核合成位点显著变化。我们使用\quokka~GPU加速代码进行了一系列高分辨率的“高盒”星际介质模拟，在其中系统地改变了星系气体表面密度、金属丰度以及不同核合成源的标高和相对速率。结果表明，不同来源产生的金属在星系风中的载荷存在显著差异，典型变化幅度约为0.3 dex，我们将这一现象称为差异金属载荷。哪种金属集合会因这一现象而优先损失取决于星系环境，且不易先验预测。我们的发现对基于丰度诊断的星系形成解释（例如恒星形成时标和初始质量函数）提出了质疑，因为这些技术所依赖的丰度变化幅度往往与我们展示的由差异金属载荷引起的幅度相当。
英文摘要：
Type Ia supernovae, type II supernovae, and asymptotic giant branch (AGB) stars are important sites of stellar nucleosynthesis, but they differ greatly in their rates, their location within a galaxy, and the mean thermal energy and abundance distribution of their ejecta. In earlier papers in this series we have shown that a significant fraction of metals newly synthesized by type II supernovae are promptly lost to galactic winds -- i.e., galactic winds are metal loaded. Here we investigate whether the elements returned by type Ia supernovae and AGB stars are similarly metal loaded, or whether metal loading varies significantly with nucleosynthetic site. We use a series of high-resolution ``tall box'' simulations of the interstellar medium with the \quokka~GPU-accelerated code, within which we systematically vary the galaxy gas surface density, metallicity, and the scale heights and relative rates of the different nucleosynthetic sources. We show that the metal loadings of galactic winds differ substantially between metals produced by different sources, with typical variations at the level of $\approx 0.3$ dex, a phenomenon we term differential metal loading. Which set of metals suffers preferential loss from this phenomenon varies depending on the galactic environment, and is not easily predictable \textit{a priori}. Our findings call into question the the interpretation of diagnostics of galaxy formation, for example star formation timescales and initial mass functions, based on abundance diagnostics, since the abundance variations upon which these techniques rely are often at levels comparable to those we show can be induced by differential metal loading.
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