论文标题
R_H = CT宇宙中的结构形成和物质功率光谱
Structure formation and the matter power-spectrum in the R_h=ct universe
论文作者
论文摘要
通货膨胀驱动量子波动以外的量子波动，使它们在辐射占主导时期的小规模模式之前将其冻结，然后衰减，而在物质后期则重新输入大规模模式，以占主导地位，并在物质时代占据主导地位。这种区别塑造了物质功率谱，并提供了观察性证据以支持标准模型。在本文中，我们证明了另一种基于R_H = CT宇宙的波动生长的机制，本身是一种FLRW宇宙学，其附加限制为零活性质量（即Rho+3p = 0），对观察到的物质功率谱也很好地说明了这一功能，因此该功能不是LambDACDM所独有的。在r_h = ct中，物质功率谱的形状是由较小模式波长的重力衰减与较大波长的较长动力学时间尺度之间的相互作用来设定的。这种组合产生的特征峰在幅度和模式数字上随时间的函数而增长。如今，该峰值约为0.02 mpc^-1，与Ly-Alpha和Planck数据一致。但是，不需要通货膨胀的扩张和复杂的时期依赖性，正如LAMBDACDM中所发现的那样。
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_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 LambdaCDM. In R_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 LambdaCDM.
