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We examine the remnant phase of radio galaxies using three-dimensionalhydrodynamical simulations of relativistic jets propagating through clusterenvironments. By switching the jets off once the lobes have reached a certainlength we can study how the energy distribution between the lobes and shockedintra-cluster medium compares to that of an active source, as well as calculatesynchrotron emission properties of the remnant sources. We see that as a resultof disturbed cluster gas beginning to settle back into the initial clusterpotential, streams of dense gas are pushed along the jet axis behind theremnant lobes, causing them to rise out of the cluster faster than they woulddue to buoyancy. This leads to increased adiabatic losses and a rapid dimming.The rapid decay of total flux density and surface brightness may explain thesmall number of remnant sources found in samples with a high flux density limitand may cause analytic models to overestimate the remnant fraction expected insensitive surveys such as those now being carried out with LOFAR.

Numerical modelling of the lobes of radio galaxies in cluster environments -- IV. Remnant radio galaxies