AI 中文总结
本文论证满足协变熵界的宇宙学模型倾向于无局域激发或单一大型黑洞的初始态，通过假设早期视界体积内充满微小黑洞衰变产生辐射，并引入随机大黑洞作为暗物质，可解释詹姆斯·韦伯望远镜观测的早期星系。
AI 中文摘要
我们论证，满足协变熵界（CEB）的宇宙学模型在数学上倾向于无局域激发或一个包含所有能量的大型黑洞的约束初始态。为了获得长的辐射主导时期，必须假设在极早期，宇宙的大多数视界体积内包含衰变为辐射的微小黑洞。两位作者之前的工作表明，这种情景可以拟合宇宙微波背景（CMB）数据。为了解释暗物质，我们还假设当时存在一些至少视界大小的随机黑洞。这种原始黑洞的合理分布可以解释所有暗物质以及詹姆斯·韦伯太空望远镜观测到的早期星系。部分暗物质也可能来自衰变黑洞的普朗克尺度残余。我们通过广义相对论的近似解和一种推测性量子引力模型来描述我们的模型，后者的流体动力学与饱和CEB的平坦$p = \pm \rho$ FRW模型相匹配。
英文摘要
We argue that cosmological models obeying the Covariant Entropy Bound (CEB) mathematically favor states with no localized excitations or one large black hole containing all the energy in a constrained initial state. In order to get a long radiation-dominated era, one must postulate that at a very early time, most horizon volumes of the universe contained tiny black holes that decayed into radiation. A previous work by two of the authors showed that such a scenario could fit the data on the Cosmic Microwave Background (CMB). In order to account for dark matter, we also postulate some random black holes of at least horizon size at that time. A reasonable distribution of such primordial black holes can account for all of dark matter as well as the early galaxies seen by the James Webb Space Telescope. Some of the dark matter may also be in Planck-scale remnants of the decaying black holes. We describe our model both in terms of approximate solutions to General Relativity and a speculative quantum gravity model whose hydrodynamics matches the flat $p = \pm ρ$ FRW model that saturates the CEB.
Comments22 pages, 6 figures, v2: revision to Appendix B, references added, v3: references added
