... description

The problem is opposite to that formulated by Wasserman (1978) and Kim et al. (1996), where the magnetic fields are expected to actively support the structure formation processes.

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...$F_{\rm G}$.

We have $F_{\rm L}/F_{\rm G} \propto \frac{H^2}{l (\rho + \delta \rho) G \rho l} \propto \frac{H^2}{\delta \rho} (\frac{t_{\rm coll}}{l})^2$, where l is the typical length scale and $t_{\rm coll}$ - the characteristic time scale of collapse. Expressing then the collapse time by the quantity used in the above notation, $t_{\rm coll} \propto \frac{1}{\delta \theta}$, one obtains for the ratio: $\frac{H^2}{\delta \rho} (\frac{1}{l \delta \theta})^2 \ll 1$ for all relevant Mpc scales of cosmological structures.

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... motion

In general relativity Kmeans the curvature index and is traditionally set to K=-1,0,+1. In Newtonian cosmology K distinguishes between different dynamical behaviours.

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... epoch

Note that the fluid velocities and not their divergences contribute to the Sachs-Wolfe temperature formula, therefore ${\Theta }_{(\rm ini)}$ is not directly determined from the CMBR satellite measurements.

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