Backflows by AGN jets: Global properties and influence on SMBH accretion
  Jets from Active Galactic Nuclei (AGN) inflate large cavities in the hot gas
environment around galaxies and galaxy clusters. The large-scale gas
circulation promoted within such cavities by the jet itself gives rise to
backflows that propagate back to the center of the jet-cocoon system, spanning
all the physical scales relevant for the AGN.
  Using an Adaptive Mesh Refinement code, we study these backflows through a
series of numerical experiments, aiming at understanding how their global
properties depend on jet parameters. We are able to characterize their mass
flux down to a scale of a few kiloparsecs to about $0.5\,\mathrm{M_\odot/y}$for
as long as $15$ or $20$ Myr, depending on jet power. We find that backflows are
both spatially coherent and temporally textbf{intermittent}, independently of
jet power in the range $10^{43-45}$ erg/s.
  Using the mass flux thus measured, we model analytically the effect of
backflows on the central accretion region, where a Magnetically Arrested Disk
lies at the center of a thin circumnuclear disk. Backflow accretion onto the
disk modifies its density profile, producing a flat core and tail.
  We use this analytic model to predict how accretion beyond the BH
magnetopause is modified, and thus how the jet power is temporally modulated.
Under the assumption that the magnetic flux stays frozen in the accreting
matter, and that the jets are always launched via the Blandford-Znajek (1977)
mechanism, we find that backflows are capable of boosting the jet power up to
tenfold during relatively short time episodes (a few Myr).
