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C. Loken (St. Mary's U.), A. Klypin (New Mexico State), G. Bryan (MIT), J. Burns (U. Missouri), M. Norman (U. Illinois/NCSA)
We present results from a statistically-complete ``catalog'' of 50 galaxy clusters simulated with a sophisticated hydro+N-body code. The simulations have high-spatial resolution (~16h-1kpc), and faithfully capture the shocks which are essential to modeling the temperature structure of clusters. Complex gas behaviour is observed including low-entropy filaments that penetrate within the outer accretion shock, large-scale outflows behind the accretion shock, and turbulent characteristics. We discuss the evolution of temperature structure and show how it can be used to discriminate between cosmological models. The evolution of the X-ray Luminosity Function (XLF) is also presented. This work was funded by NASA and NSF.