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We present results from a suite of binary merging cluster simulations. Thehydrodynamical cluster simulations are performed employing a smoothed particlehydrodynamics (SPH) formulation in which gradient errors are strongly reducedby means of an integral approach. We consider adiabatic as well as radiativesimulations, in which we include gas cooling, star formation and energyfeedback from supernovae. We explore the effects of merging on thethermodynamic structure of the intracluster gas of the final merger remnant. Inparticular, we study how core entropy is generated during the merging and thestability properties of the initial cool-core profile against disruption. Tothis end, we consider a range of initial mass ratio and impact parameters.Final entropy profiles of our adiabatic merging simulations are in good accordwith previous findings (ZuHone 2011), with cool-cores being disrupted for allof the initial merging setups. For equal-mass off-axis mergers, we find that asignificant contribution to the final primary core entropy is due tohydrodynamic instabilities generated by rotational motions, which are inducedby tidal torques during the first pericenter passage. In radiative simulations,cool-cores are more resilient against heating processes; nonetheless, they areable to maintain their integrity only in the case of off-axis mergers with veryunequal masses. We suggest that these results are robust against changes in thegas physical modeling, in particular to the inclusion of AGN thermal feedback.  Our findings support the view that the observed core cluster morphologyemerges naturally in a merging cluster context, and conclude that the mergingangular momentum is a key parameter in shaping the thermodynamical propertiesof the final merger remnant.

A study of cool core resiliency and entropy mixing in simulations of galaxy cluster mergers