  By means of N-body/hydrodynamical simulations we model the evolution of a
primordial 10^{8} solar masses density peak which ends up in an object closely
resembling the present day globular cluster Omega Centauri. We succeed to
reproduce the main features of the cluster, namely the structure, kinematics
and metallicity distribution. We suggest that Omega Centauri might be a
cosmological dwarf elliptical, formed at high redshift, evolved in isolation
and self-enriched, and eventually fallen inside the potential well of the Milky
Way, in agreement with the Searle-Zinn (1978) paradigm for galactic globular
clusters formation. We finally suggest that Omega Centauri is probably
surrounded by an extended Dark Matter (DM) halo, for which no observational
evidence is at present available. We expect that signatures, if any, of the DM
halo can be found in the kinematics of stars outside about 20 arcmin.
