  We investigate the role of radiative cooling within the core of large X-ray
clusters using multi-phase hydrodynamics. We developed for that purpose a
spherically symmetric hydrodynamical code, coupled to a "fluid model" that
describes accurately the dark matter component. Cooling is included using a
self-consistent multi-phase approach, leading to "cooled gas" mass deposition
throughout the flow. We simulate the collapse and the subsequent evolution of a
Coma-like X-ray cluster, avoiding the well-known "cooling catastrophe". The
total mass profile of our simulated cluster is very similar to the "universal"
profile proposed by Navarro, Frenk & White (1995). More interestingly, we also
obtain a quasi-isothermal temperature profile, which is a direct consequence of
multi-phase cooling within such a potential well.
