第一批恒星的自洽半解析模型
Self-consistent semi-analytic models of the first stars
摘要：
我们已经开发了一个半分析框架来模拟第一个第三星族（Pop III）恒星的大规模演化和向富含金属的恒星形成的过渡。我们的模型遵循宇宙学N体模拟的暗物质晕，利用它们各自的合并历史和三维位置，并应用物理激励的处方恒星形成和反馈莱曼-沃纳（LW）辐射，氢电离辐射和外部金属富集由于超新星风。这种方法的目的是补充分析研究，其中不包括集群或个人合并的历史，流体动力学宇宙学模拟，其中包括详细的物理，但计算昂贵，动态范围有限。利用这种技术，我们计算的累积Pop III和金属富集的恒星形成率密度（SFRD）的红移在$z \geq 20$的函数。我们发现，不同的模型参数会导致显着的全球恒星形成历史的质的变化。Pop III恒星形成效率和Pop III与随后的金属富集恒星形成之间的延迟时间被认为具有最大的影响。聚类（即包括个人晕的三维位置）对各种反馈机制的影响也进行了研究。在我们的基准模型中，集群对LW和电离反馈的影响相对温和，但如果外部金属富集可以促进金属富集恒星在大距离上形成，则影响可能更大。
英文摘要：
We have developed a semi-analytic framework to model the large-scale evolution of the first Population III (Pop III) stars and the transition to metal-enriched star formation. Our model follows dark matter halos from cosmological N-body simulations, utilizing their individual merger histories and three-dimensional positions, and applies physically motivated prescriptions for star formation and feedback from Lyman-Werner (LW) radiation, hydrogen ionizing radiation, and external metal enrichment due to supernovae winds. This method is intended to complement analytic studies, which do not include clustering or individual merger histories, and hydrodynamical cosmological simulations, which include detailed physics, but are computationally expensive and have limited dynamic range. Utilizing this technique, we compute the cumulative Pop III and metal-enriched star formation rate density (SFRD) as a function of redshift at $z \geq 20$. We find that varying the model parameters leads to significant qualitative changes in the global star formation history. The Pop III star formation efficiency and the delay time between Pop III and subsequent metal-enriched star formation are found to have the largest impact. The effect of clustering (i.e. including the three-dimensional positions of individual halos) on various feedback mechanisms is also investigated. The impact of clustering on LW and ionization feedback is found to be relatively mild in our fiducial model, but can be larger if external metal enrichment can promote metal-enriched star formation over large distances.
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