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On long wavelengths the gradient term is negligible. The Friedmann equation impliesDuring matter domination, $a\propto t^{2/3}$ and $H=2/(3t)$, so the linear growth equation becomesThe power-law ansatz $\delta \propto t^s$ gives $s=2/3$ or $s=-1$. Since $a\propto t^{2/3}$, the growing and decaying modes are

During matter domination, $4\pi G{\bar{\rho }}_m=3H^2/2$ and $a\propto t^{2/3}$. Substitution of ${\delta }_m\propto t^p$ gives $p=2/3,-1$, henceDuring radiation domination, neglecting the rapidly oscillating radiation perturbation and the subdominant matter source leavesThereforeThis logarithmic behavior is the Mészáros effect for subhorizon cold dark matter.

In a radiation-dominated background with matter self-gravity retained, ${\delta }_{aa}+{\delta }_a/a-3\delta /(2a{a}_{\mathrm{eq}})=0$. A change to $x=\sqrt{6a/a_{\mathrm{eq}}}$ gives the Modified Bessel differential equation of order zero. The Modified Bessel function of the first kind increases as $1+3a/(2a_{\mathrm{eq}})+\cdots$; the Modified Bessel function of the second kind decreases with a leading negative logarithm. The early solution space has the constant/logarithmic behaviors, not the $a$ growth of matter domination. This background approximation must not be extrapolated through equality.

In a flat universe containing separately conserved radiation in cosmology and pressureless matter, the Friedmann equation becomes $(a^{\prime }{)}^2=H_0^2({\Omega }_{r,0}+{\Omega }_{m,0}a)$ in conformal time. Setting $a=0$ at $\tau =0$ gives the stated quadratic-plus-linear scale factor. The linear term controls radiation domination and the quadratic term controls matter domination. The formula presumes $a_0=1$, ${\Omega }_{r,0}+{\Omega }_{m,0}=1$ and no cosmological constant.

The matter equation in the barotropic matter-string model contains no wavenumber. Growing initial data therefore evolve as ${\delta }_c(k,\eta )=A_{k}D(\eta )$ with the same $D$ for every mode. For regular adiabatic modes initially outside the horizon during matter domination, $A_k$ is proportional to $k^2$ times the primordial curvature amplitude. The density-per-curvature transfer is consequently proportional to $k^{2}D(\eta )$ for modes entering after equality. Factoring out both $k^2$ and $D$ gives a constant shape transfer on those scales. Comparing with continued matter-era growth instead introduces the common suppression $D(\eta )/\eta$, not a new wavenumber dependence.

For last scattering well inside matter domination, $c_s=c/\sqrt{3}$ gives physical sound radius $R_s=2c{a}_{\ast }^{3/2}/(\sqrt{3}{H}_0\sqrt{{\Omega }_m})$. Neglecting the early conformal time in the observer distance, an open dust cosmology has transverse comoving last-scattering distance $r_{\ast }=2c/(H_0{\Omega }_m)$. Thus ${\theta }_s=R_s/(a_{\ast }{r}_{\ast })=\sqrt{{\Omega }_m{a}_{\ast }/3}$ and $\ell \sim \pi /{\theta }_s$. Radiation, baryon sound-speed evolution and acoustic phase shifts refine this estimate.

// Target: cosmology.bigb

A residual synchronous time displacement ${\xi }^0=C(\mathbf{x})/a$ changes a fluid density contrast by $-{\bar{\rho }}^{\prime }{\xi }^0/\bar{\rho }$. For constant equation of state this gives the displayed mode: it scales as ${\tau }^{-2}$ during radiation domination and as ${\tau }^{-3}$ during matter domination. Such density changes alone do not indicate physical structure growth. Choosing the cold-matter rest frame fixes the residual time displacement, while a spatial relabeling fixes the remaining integration convention for the metric trace.