  We present a new set of dissipationless N-body simulations aiming to better
understand the pure dynamical aspects of the ``Fundamental Plane'' (FP) of
elliptical galaxies. We have extended our previous hierarchical merger scheme
by considering the Hernquist profile for the initial galaxy model.
Two-component Hernquist galaxy models were also used to study the effect of
massive dark halos on the end-products characteristics. We have also performed
new collapse simulations including initial spin. We found that the
one-component Hernquist mergers give results similar to those found for the
one-component King models, namely both were able to build-up small scatter
FP-like correlations with slopes consistent with what is found for the
near-infrared FP of nearby galaxies. The two-component models also reproduce a
FP-like correlation, but with a significantly steeper slope. This is in
agreement with what has been found for elliptical galaxies at higher redshift
(0.1 $<$ z $<$ 0.6). We discuss some structural properties of the simulated
galaxies and their ability to build-up FP-like correlations. We confirm that
collapses generally do not follow a FP-like correlation regardless of the
initial spin. We suggest that the evolution of gradients in the gravitational
field of the merging galaxies may be the main ingredient dictating the final
non-homology property of the end products.
