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C. Loken (CITA), M. Norman, E. Nelson (UCSD), J. Burns (U. Missouri), A. Klypin (NMSU), G. Bryan (MIT)
We investigate the temperature structure of the hot, X-ray emitting gas in a numerically-simulated ``catalogue" of clusters of galaxies at z=0 in a flat, \LambdaCDM universe (\Omegab = 0.026, \Omega\Lambda=0.7, h=0.7). The high-resolution (15h-1kpc) simulations make use of a sophisticated, Eulerian-based, Adaptive Mesh-Refinement (AMR) code which faithfully captures the shocks that are essential to modelling the temperature structure of clusters. We find that the temperature structure on Mpc-scales is highly complex and non-isothermal. Both the 3D and 2D temperature profiles of these clusters decrease by a factor of (2-3) from the cluster core to half the virial radius (~1h-1Mpc). This decrease is in good agreement with the observational results of Markevitch et al. (1998). We discuss the interpretation of this result and make predictions for XMM. This work was funded by NASA and NSF.