Inner structure of dark matter halos at high <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>z</mml:mi></mml:math> in cosmological models with non-power-law primordial spectra

We consider three cosmological models with non-power-law spectra of primordial density perturbations and test them against $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ in density profiles of dark matter halos. We found that, despite the significant difference in initial conditions, the mean density profiles of all models are still close to the Navarro-Frenk-White one, albeit with some dispersion. We demonstrate that the density profile slopes in the innermost part of the halo have a significant evolution with $z$, which can be used to identify the cosmological model. We also present a toy model resulting in the appearance of core in the central part of the dark matter halo.