  Aims:In this study we investigate the evolution of shape and kinematics of
elliptical galaxies in a cosmological framework.
  Methods: We use a set of hydrodynamic, self-consistent simulations operating
in the context of a concordance cosmological model where relaxed
elliptical-like objects (ELOs) were identified at redshifts z=0, z=0.5, z=1 and
z=1.5.
  Results: The population of elliptical systems analysed here present a
systematic change through time, i.e. evolution, by becoming rounder in general
at z=0 and, at the same time more velocity dispersion supported. This is found
to be primarily due to major dry mergers where only a modest amount of angular
momentum is involved into the merger event. Despite the general trend, in a
significant amount of cases the merger event involves a higher specific angular
momentum, which in general causes the system to acquire a higher rotational
support and/or a more oblate shape. These evolutionary patterns are still
present when we study our systems in projection, mimicking real observations,
and thus they should become apparent in future observations.
