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Inflation drives quantum fluctuations beyond the Hubble horizon, freezingthem out before the small-scale modes re-enter during the radiation dominatedepoch, and subsequently decay, while large-scale modes re-enter later duringthe matter dominated epoch and grow. This distinction shapes the matter powerspectrum and provides observational evidence in support of the standard model.In this paper, we demonstrate that another mechanism, based on the fluctuationgrowth in the R_h=ct universe, itself an FLRW cosmology with the addedconstraint of zero active mass (i.e., rho+3p=0), also accounts very well forthe 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 interplaybetween the more rapid decay of the gravitational potential for the smallermode wavelengths and the longer dynamical timescale for the larger wavelengths.This combination produces a characteristic peak that grows in both amplitudeand mode number as a function of time. Today, that peak lies at k approx 0.02Mpc^-1, in agreement with the Ly-alpha and Planck data. But there is no need ofan inflationary expansion, and a complicated epoch dependence as one finds inLambdaCDM.

Structure formation and the matter power-spectrum in the R_h=ct universe