The description of spacetime is an fundamental problem of cosmology. We explain why the current assignments of spacetime geometries for ${\Omega }_k$ of the Friedmann-Lemaître-Robertson-Walker (FLRW) model are probably incorrect and suggest more useful descriptions. We show that ${\Omega }_k$ represents not only curvature but the influence of matter density on the extent of spacetime between massive objects. Recent analyses of supernovae type Ia (SNe Ia) and HII/GEHR data with the FLRW model present the best fits with a small value for ${\Omega }_m$ and a large ${\Omega }_k$. These results are consistent with our Universe exhibiting sparse matter density and quasi-Euclidean geometry and the small ${\Omega }_m$ value agrees with Big Bang nucleosynthesis calculations. We suggest the geometry of our current Universe is better described by a value for ${\Omega }_k\approx$1 rather than 0. As an example we extend the FLRW model towards the Big Bang and discover a simple explanation of how matter creation developed into the currently geometrically flat Universe with sparse, homogeneous, isotropic matter and energy distributions. Assigning ${\Omega }_k\approx 1$ to describe quasi-Euclidean spacetime geometry is also useful for estimating $H_0$ and should help resolve the “tension” surrounding current estimates by different investigators.

时空的描述是宇宙学的一个基本问题。我们解释了为什么当前时空几何的分配${\Omega }_{ķ}$Friedmann-Lemaître-Robertson-Walker（FLRW）模型的模型可能不正确，并提出了更有用的描述。我们证明${\Omega }_{ķ}$不仅表示曲率，而且表示物质密度对大型物体之间时空范围的影响。最近用FLRW模型对Ia型超新星（SNe Ia）和HII / GEHR数据进行的分析显示了最佳拟合，且拟合值较小${\Omega }_{米}$ 和一个大 ${\Omega }_{ķ}$。这些结果与我们的宇宙显示稀疏物质密度和准欧几里得几何以及小${\Omega }_{米}$该值与Big Bang核合成计算相符。我们建议用的值更好地描述当前宇宙的几何形状${\Omega }_{ķ}\approx$1而不是0。作为示例，我们将FLRW模型扩展到“大爆炸”，并发现了一个简单的解释，即物质创造如何发展为具有稀疏，均质，各向同性物质和能量分布的当前几何平坦的宇宙。分配${\Omega }_{ķ}\approx \mathrm{1个}$ 描述拟欧几里德时空几何也可用于估算 $H_0$ 并应有助于解决不同研究者当前估计的“压力”。