Growth of Dark Matter Perturbations during Kination
  If the Universe's energy density was dominated by a fast-rolling scalar field
while the radiation bath was hot enough to thermally produce dark matter, then
dark matter with larger-than-canonical annihilation cross sections can generate
the observed dark matter relic abundance. To further constrain these scenarios,
we investigate the evolution of small-scale density perturbations during such a
period of kination. We determine that once a perturbation mode enters the
horizon during kination, the gravitational potential drops sharply and begins
to oscillate and decay. Nevertheless, dark matter density perturbations that
enter the horizon during an era of kination grow linearly with the scale factor
prior to the onset of radiation domination. Consequently, kination leaves a
distinctive imprint on the matter power spectrum: scales that enter the horizon
during kination have enhanced inhomogeneity. We also consider how matter
density perturbations evolve when the dominant component of the Universe has a
generic equation-of-state parameter $w$. We find that matter density
perturbations do not grow if they enter the horizon when ${0< w < 1/3}$. If
matter density perturbations enter the horizon when ${w > 1/3}$, their growth
is faster than the logarithmic growth experienced during radiation domination.
The resulting boost to the small-scale matter power spectrum leads to the
formation of enhanced substructure, which effectively increases the dark matter
annihilation rate and could make thermal dark matter production during an era
of kination incompatible with observations.
