Reionization in the Light of Dark Stars
Reionization in the Light of Dark Stars
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DOI：
10.3847/1538-4357/ac7fea
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发表时间：
2021-12
期刊：
影响因子：
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通讯作者：
P. Gondolo;Pearl Sandick;Barmak Shams Es Haghi;E. Visbal
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文献类型：
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作者：
P. Gondolo;Pearl Sandick;Barmak Shams Es Haghi;E. Visbal
我们研究了暗星 (DS) 对宇宙再电离历史的影响，以及暗星与莱曼-沃纳 (LW) 辐射反馈之间的相互作用，将宇宙微波背景 (CMB) 光学深度降低到普朗克测量的 τ = 0.054 ± 0.007 范围内的值。我们使用半解析方法来评估再电离历史和 CMB 光学深度，其中包括原子冷却晕中的族 II 恒星和具有 LW 反馈的迷你晕中的族 III 恒星，之前是 DS 阶段。我们表明，虽然只有当族 III 恒星形成效率小于 ∼0.2% 时，LW 反馈本身才能将到最后散射表面的集成光学深度降低到 ∼0.05，但包含 DS 族可以自然地导致测量到的 CMB 光学深度，从而获得更大的族 III 恒星形成效率 ≳1%。
We investigate the effect of dark stars (DSs) on the reionization history of the universe, and the interplay between them and feedback due to Lyman–Werner (LW) radiation in reducing the cosmic microwave background (CMB) optical depth to a value within the τ = 0.054 ± 0.007 range measured by Planck. We use a semianalytic approach to evaluate reionization histories and CMB optical depths, which includes Population II stars in atomic cooling halos and Population III stars in minihalos with LW feedback, preceded by a DS phase. We show that while LW feedback by itself can reduce the integrated optical depth to the last scattering surface to ∼0.05 only if the Population III star formation efficiency is less than ∼0.2%, the inclusion of a population of DSs can naturally lead to the measured CMB optical depth for much larger Population III star formation efficiencies ≳1%.