  We perform N-body simulations for models with a DE component. Besides of DE
with constant negative state parameter w, we consider DE due to scalar fields,
self-interacting through RP or SUGRA potentials. According to our post-linear
analysis, at z=0, DM power spectra and halo mass functions do not depend on DE
nature. This is welcome, as LCDM fits observations. Halo profiles, instead, are
denser than LCDM. For example, the density at 15 kpc of a DE halo with M=10^13
exceeds LCDM by ~45%. Differences, therefore, are small but, however, DE does
not ease the problem with cuspy DM profiles. We study also subhalos and find
that, at $z=0$, the number of satellites coincides in all DE models. At higher
z, DE models show increasing differences from LCDM and among themselves (i.e.
in the mass function evolution); this is the obvious pattern to distinguish
between different DE state equations.
