  We present numerical simulations investigating the interaction of AGN jets
with galaxy clusters, for the first time taking into account the dynamic nature
of the cluster gas and detailed cluster physics. The simulations successfully
reproduce the observed morphologies of radio sources in clusters. We find that
cluster inhomogeneities and large scale flows have significant impact on the
morphology of the radio source and cannot be ignored a-priori when
investigating radio source dynamics. Morphological comparison suggests that the
gas in the centres of clusters like Virgo and Abell 4059 shows significant
shear and/or rotation. We find that shear and rotation in the intra-cluster
medium move large amounts of cold material back into the path of the jet,
ensuring that subsequent jet outbursts encounter a sufficient column density of
gas to couple with the inner cluster gas, thus alleviating the problem of
evacuated channels discussed in the recent literature. The same effects
redistribute the excess energy Delta_E deposited by the jets, making the
distribution of Delta_E at late times consistent with being isotropic.
