Inflation drives quantum fluctuations beyond the Hubble horizon, freezing them out before the small-scale modes re-enter during the radiation dominated epoch, and subsequently decay, while large-scale modes re-enter later during the matter dominated epoch and grow. This distinction shapes the matter power spectrum and provides observational evidence in support of the standard model. In this paper, we demonstrate that another mechanism, based on the fluctuation growth in the $R_{\mathrm{h}}=ct$ universe, itself an FLRW cosmology with the added constraint of zero active mass (i.e., $\rho +3p=0$), also accounts very well for the observed matter power spectrum, so this feature is not unique to $\Lambda$CDM. In $R_{\mathrm{h}}=ct$, the shape of the matter power spectrum is set by the interplay between the more rapid decay of the gravitational potential for the smaller mode wavelengths and the longer dynamical timescale for the larger wavelengths. This combination produces a characteristic peak that grows in both amplitude and mode number as a function of time. Today, that peak lies at $k\approx 0.02$ Mpc⁻¹, in agreement with the Ly-$\alpha$ and Planck data. But there is no need of an inflationary expansion, and a complicated epoch dependence as one finds in $\Lambda$CDM.

通货膨胀使量子涨落超出哈勃的视界，在辐射主导的时代之前小尺度模式重新进入之前将其冻结，然后衰减，而物质主导的时代之后较大模式又重新进入并增长。这种区别塑造了物质功率谱，并提供了支持标准模型的观察证据。在本文中，我们证明了另一种机制是基于${\mathrm{[R}}_{\mathrm{H}}=CŤ$ 宇宙本身就是FLRW宇宙学，附加了零有效质量约束（即， $\rho +3p=0$），也很好地说明了观测物质的功率谱，因此该功能并非唯一 $\Lambda$CDM。在${\mathrm{[R}}_{\mathrm{H}}=CŤ$物质功率谱的形状是由较小模式波长的引力势的较快衰减与较大波长的较长的动力时标之间的相互作用决定的。这种组合会产生一个特征峰，该峰的振幅和模式数均随时间而变。今天，那个高峰在$ķ\approx 0。02$Mpc ^-1，与Ly-同意$\alpha$和普朗克数据。但是没有必要进行通货膨胀扩张，而且人们会发现复杂的历时依赖性$\Lambda$CDM。