  We present results of an analysis of the structural and kinematical
properties of a sample of elliptical-like objects (ELOs) identified in four
hydrodynamical, self-consistent simulations run with the DEVA code (Serna et
al. 2003). Star formation has been implemented in the code through a simple
phenomenological parameterization, that takes into account stellar physics
processes only implicitly through the values of a threshold gas density,
$\rho_{\rm g,thres}$, and an efficiency parameter, $c_*$. The four simulations
operate in the context of a $\Lambda$CDM cosmological model consistent with
observations, resolve ELO mass assembly at scales up to $\simeq$ 2 kpc, and
differ in the values of their star formation parameters. Stellar masses,
projected half-mass radii and central l.o.s. velocity dispersions, $\sigma_{\rm
los, 0}$, have been measured on the ELO sample and their values compared with
data from the Sloan digital sky survey. For the first time in self-consistent
simulations, a good degree of agreement has been shown, including the
Faber-Jackson and the $D_n - \sigma_{\rm los, 0}$ relations, among others, but
only when particular values of the $\rho_{\rm g,thres}$ and $c_*$ parameters
are used. This demostrates the effect that the star formation parameterization
has on the ELO mass distribution. Additionally, our results suggest that it is
not strictly necessary, at the scales resolved in this work, to appeal to
energy sources other than gravitational (as for example supernovae feedback
effects) to account for the structure and kinematics of large ellipticals.
