| Details: |
Abstract:
It has been well established that feedback from the central super-massive black holes is an essential ingredient in galaxy evolution. However, how exactly they affect the gas both within the host galaxy and its nearby environment, over what spatial and time scales remains an open question. I shall present the results of our recent 3D relativistic (magneto) hydrodynamic simulations, performed on scales of several kiloparsecs, of relativistic jets from AGNs interacting with the turbulent interstellar medium of the host galaxy and the ambient circumgalactic medium. In the early phase of its evolution, the jets remain frustrated within the dense ISM, shocking it over scales much larger than its apparent size. The nature of the interaction depends on several parameters such as jet power, ambient density and morphology of the gas. The jets can potentially enhance star-formation at sites of direct interaction. However, the enhanced turbulence induced at larger scales can also reduce the SFR. I will discuss the potential implications of these results on the evolutionary history of the galaxy, and the observational signatures predicted by our simulations which support previous observed results of jet feedback and more recent confirmations of wide scale jet feedback through emission line studies.
|