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We present predictions for the evolution of radio emission from ActiveGalactic Nuclei (AGNs). We use a model that follows the evolution ofSupermassive Black Hole (SMBH) masses and spins, within the latest version ofthe GALFORM semi-analytic model of galaxy formation. We use a Blandford-Znajektype model to calculate the power of the relativistic jets produced by blackhole accretion discs, and a scaling model to calculate radio luminosities.First, we present the predicted evolution of the jet power distribution,finding that this is dominated by objects fuelled by hot halo accretion and anADAF accretion state for jet powers above $10^{32}\mathrm{W}$ at $z=0$, withthe contribution from objects fuelled by starbursts and in a thin discaccretion state being more important for lower jet powers at $z=0$ and at alljet powers at high redshifts ($z\geq3$). We then present the evolution of thejet power density from the model. The model is consistent with currentobservational estimates of jet powers from radio luminosities, once we allowfor the significant uncertainties in these observational estimates. Next, wecalibrate the model for radio emission to a range of observational estimates ofthe $z=0$ radio luminosity function. We compare the evolution of the modelradio luminosity function to observational estimates for $0<z<6$, finding thatthe predicted evolution is similar to that observed. Finally, we explorerecalibrating the model to reproduce luminosity functions of core radioemission, finding that the model is in approximate agreement with theobservations.

The evolution of radio jets across cosmic time