  We present a series of cosmological N-body simulations which make use of the
hydrodynamic approach to the evolution of structures (Dominguez 2000). This
approach addresses explicitly the existence of a finite spatial resolution and
the dynamical effect of subresolution degrees of freedom. We adapt this method
to cosmological simulations of the standard LCDM structure formation scenario
and study the effects induced at redshift z=0 by this novel approach on the
large-scale clustering patterns as well as (individual) dark matter halos.
Comparing these simulations to usual N-body simulations, we find that (i) the
new (hydrodynamic) model entails a proliferation of low--mass halos, and (ii)
dark matter halos have a higher degree of rotational support. These results
agree with the theoretical expectation about the qualitative behaviour of the
"correction terms" introduced by the hydrodynamic approach: these terms act as
a drain of inflow kinetic energy and a source of vorticity by the small-scale
tidal torques and shear stresses.
