The Impact of Black Hole Formation on Population-averaged Supernova Yields
The Impact of Black Hole Formation on Population-averaged Supernova Yields
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DOI：
10.3847/1538-4357/ac1bac
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发表时间：
2021-03
期刊：
影响因子：
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通讯作者：
Emily J. Griffith;T. Sukhbold;D. Weinberg;Jennifer A. Johnson;James W. Johnson;F. Vincenzo
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作者：
Emily J. Griffith;T. Sukhbold;D. Weinberg;Jennifer A. Johnson;James W. Johnson;F. Vincenzo
黑洞（BH）形成的景观，其中大质量的恒星爆炸的核心坍缩超新星（CCSN），并内爆成BH深刻地影响初始质量函数（IMF）平均核合成产量的恒星人口。在Sukhbold等人工作的基础上，我们计算了各种假设条件下太阳金属丰度的IMF平均产额，这些假设条件包括具有广泛BH形成的中微子驱动发动机模型、具有BH形成的简单质量阈值的模型，以及一个8到120 M质量的所有恒星都爆炸的模型。对于合理的选择，α元素的总产额跨越3倍，但相对产额的变化更微妙，通常为0.05-0.2倍。为了限制BH形成的总体水平，C和N与O或Mg的比率是有希望的诊断。为了区分复杂的，理论上动机的景观从简单的质量阈值，丰度比涉及锰或镍是有希望的，因为它们的敏感性的核心结构的CCSN祖。我们证实了以前的研究结果预测的O/Mg产率比和观测推断的值之间的差异很大（因子2.5-4），这意味着模型要么过量生产O或生产不足镁。没有景观选择实现全面的协议与观察到的丰度比;差异提供经验线索的方面大质量星星演化或爆炸物理仍然缺少的模型。我们发现定性相似的结果使用大质量星星收益率的Limongi和Chieffi。我们提供了几种景观方案的IMF集成产量表，更灵活的用户设计的模型可以通过公开的化学进化通用积分器（VICE; https：//pypi.org/project/vice/）来实现。
The landscape of black hole (BH) formation—in which massive stars explode as core-collapse supernovae (CCSN) and which implode into BHs—profoundly affects the initial-mass-function (IMF)-averaged nucleosynthetic yields of a stellar population. Building on the work of Sukhbold et al., we compute IMF-averaged yields at solar metallicity for a wide range of assumptions, including neutrino-driven engine models with extensive BH formation, models with a simple mass threshold for BH formation, and a model in which all stars from 8 to 120 M ⊙ explode. For plausible choices, the overall yields of α-elements span a factor of 3, but changes in relative yields are more subtle, typically 0.05–0.2 dex. To constrain the overall level of BH formation, ratios of C and N to O or Mg are promising diagnostics. To distinguish complex, theoretically motivated landscapes from simple mass thresholds, abundance ratios involving Mn or Ni are promising because of their sensitivity to the core structure of the CCSN progenitors. We confirm previous findings of a substantial (factor 2.5–4) discrepancy between predicted O/Mg yield ratios and observationally inferred values, implying that models either overproduce O or underproduce Mg. No landscape choice achieves across-the-board agreement with observed abundance ratios; the discrepancies offer empirical clues to aspects of massive star evolution or explosion physics still missing from the models. We find qualitatively similar results using the massive star yields of Limongi & Chieffi. We provide tables of IMF-integrated yields for several landscape scenarios, and more flexible user-designed models can be implemented through the publicly available Versatile Integrator for Chemical Evolution (VICE; https://pypi.org/project/vice/).