论文标题
通过结构形成引起的曲率求解曲率和哈勃参数不一致
Solving the curvature and Hubble parameter inconsistencies through structure formation-induced curvature
论文作者
论文摘要
最近，Di Valentino，Melchiorri和Silk（2019）指出的是，增强的镜头信号相对于在空间平坦的$λ$ CDM模型中的预期构成了可能的危机，这可能是Friedmann-Lema \^iTre-Robertson-Walker（FLRRW）类型的类模型类别的危机。当flrw曲率参数$ω_{k0} $从数据确定而不是约束为零以零为零时，“危机”等于宇宙学数据集之间的不一致。此外，由普朗克确定的哈勃参数与本地观察结果之间已经实质性的差异增加到$5σ$的水平。尽管这种不一致可能是由于在小角度尺度上影响普朗克宇宙微波背景（CMB）功率谱的天体物理起源的系统效应，但这是一种选择，是由于FLRW假设的失败所致。在本文中，我们回想起了FLRW曲率Ansatz如何被预期因通用相对论时间而违反。我们解释了如何通过结构形成来修改体积平均空间曲率的FLRW保护方程，并在一个简单的框架中说明了如何解决FLRW时空中的曲率张力如何从一般相对论的角度来解决 - 甚至可以预期发生。需要与空间曲率参数$ω__{K0} $相当于Planck Power Spectra优先的早期时间收敛，该模型具有空间曲率参数$ω_{K0} $。
Recently it has been noted by Di Valentino, Melchiorri and Silk (2019) that the enhanced lensing signal relative to that expected in the spatially flat $Λ$CDM model poses a possible crisis for the Friedmann-Lema\^ıtre-Robertson-Walker (FLRW) class of models usually used to interpret cosmological data. The 'crisis' amounts to inconsistencies between cosmological datasets arising when the FLRW curvature parameter $Ω_{k0}$ is determined from the data rather than constrained to be zero a priori. Moreover, the already substantial discrepancy between the Hubble parameter as determined by Planck and local observations increases to the level of $5σ$. While such inconsistencies might arise from systematic effects of astrophysical origin affecting the Planck Cosmic Microwave Background (CMB) power spectra at small angular scales, it is an option that the inconsistencies are due to the failure of the FLRW assumption. In this paper we recall how the FLRW curvature ansatz is expected to be violated for generic relativistic spacetimes. We explain how the FLRW conservation equation for volume-averaged spatial curvature is modified through structure formation, and we illustrate in a simple framework how the curvature tension in a FLRW spacetime can be resolved -- and is even expected to occur -- from the point of view of general relativity. Requiring early-time convergence towards a Friedmannian model with a spatial curvature parameter $Ω_{k0}$ equal to that preferred from the Planck power spectra resolves the Hubble tension within our dark energy-free model.
