Results from a large set of hydrodynamical SPH simulations
of galaxy clusters in a flat LCDM cosmology are used to investigate
cluster X-ray properties. The physical modeling of the gas includes radiative
cooling, star formation, energy feedback and metal enrichment that
follows from the explosions of SNe type II and Ia.
The metallicity dependence of the cooling function is also taken into account.
It is found that the luminosity-temperature relation of simulated clusters
is in good agreement with the data, and the X-ray properties of cool
clusters are unaffected by the amount of feedback energy that has heated the
intracluster medium (ICM). The fraction of hot gas $f_g$ at the virial radius
increases with $T_X$
and the distribution obtained from the simulated cluster sample is consistent
with the observational ranges.
