AGN feedback is widely considered the major heating source to prevent a classical cooling flow in the center of galaxy clusters. Numerical simulations have shown that momentum-driven AGN feedback can suppress cooling successfully and reproduce cluster properties generally in good agreement with the observations. However, exactly how the jet is coupled to the intra-cluster medium is still unclear. In this work, we study how much heating comes from shock waves, and how much from turbulent dissipation in a simulation where cooling is balanced by AGN feedback. We also examine how the importance of different heating processes changes as a function of time, distance to the center, and the thermal properties of the gas.