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Energy deposition by active galactic nuclei jets into the ambient medium canaffect galaxy formation and evolution, the cooling of gas flows at the centresof galaxy clusters, and the growth of the supermassive black holes. However,the processes that couple jet power to the ambient medium and determine jetmorphology are poorly understood. For instance, there is no agreement on thecause of the well-known Fanaroff-Riley (FR) morphological dichotomy of jets,with FRI jets being shorter and less stable than FRII jets. We carry out global3D magnetohydrodynamic simulations of relativistic jets propagating through theambient medium. We show that the flat density profiles of galactic cores slowdown and collimate the jets, making them susceptible to the 3D magnetic kinkinstability. We obtain a critical power, which depends on the galaxy core massand radius, below which jets become kink-unstable within the core, stall, andinflate cavities filled with relativistically-hot plasma. Jets above thecritical power stably escape the core and form powerful backflows. Thus, thekink instability controls the jet morphology and can lead to the FR dichotomy.The model-predicted dependence of the critical power on the galaxy opticalluminosity agrees well with observations.

Three-dimensional Relativistic MHD Simulations of Active Galactic Nuclei Jets: Magnetic Kink Instability and Fanaroff-Riley Dichotomy