  In this work, we extend the model proposed by White concerning the
post-collapse evolution of density peaks while considering the role of angular
momentum. On a timescale smaller than the peak collapse, $t_{0}$, the inner
regions of the peak reach the equilibrium forming a cuspy profile, as in
White's paper, but the power-law density profile is flatter, namely $\rho
\propto r^{-1.52}$, using the specific angular momentum $J$ obtained in
theoretical models of how it evolves in CDM universes, namely $J \propto
M^{2/3}$. The previous result shows how angular momentum influences the slope
of the density profile, and how a slightly flatter profile obtained in
high-resolution numerical simulations, namely $\rho \propto r^{\alpha}$,
$(\alpha \simeq -1.5)$ can be reobtained. Similarly to simulations, in our
model adiabatic contraction was not taken into account. This means that more
comprehensive simulations could give different values for the slope of the
density profile, similar to an improvement of our model.
