  We present some of the results of an ongoing collaboration to sudy the
dynamical properties of galaxy clusters by means of high resolution adiabatic
SPH cosmological simulations. Results from our numerical clusters have been
tested against analytical models often used in X-ray observations: $\beta$
model (isothermal and polytropic) and those based on universal dark matter
profiles. We find a universal temperature profile, in agreement with AMR
gasdynamical simulations of galaxy clusters. Temperature decreases by a factor
2-3 from the center to virial radius. Therefore, isothermal models (e.g.
$\beta$ model) give a very poor fit to simulated data. Moreover, gas entropy
profiles deviate from a power law near the center, which is also in very good
agreement with independent AMR simulations. Thus, if future X-ray observations
confirm that gas in clusters has an extended isothermal core, then
non-adiabatic physics would be required in order to explain it.
