  We conducted 3D-MHD simulations to investigate the feedback processes in the
central 1kpc scale of galaxies hosting both active star formation (SF) and an
AGN wind. Our simulations naturally generated a turbulent and clumpy
interstellar medium driven by SF evolution. We found that the AGN wind duty
cycle plays a crucial role in shaping the evolution of the outflows. This cycle
consists of an active, a remnant and an inactive phase, lasting up to 1.5 Myr.
The duration of the cycle increases with larger star formation rate (SFR) and
smaller AGN wind power (tested for luminosities log L = 42-44 ergs per second
and SFR=1-1000 solar masses per year. The feedback on SF, whether positive or
negative, depends on various factors, including the AGN outflow opening angle,
power, and phase of activity, as well as the initial SFR. The passage of the
AGN wind enhances SF in a ring around it, resembling the structures observed in
ULIRGs, and is stronger for larger AGN power or SFR. Also, a higher SFR
enhances the mixing of interstellar matter with the AGN wind, resulting in a
greater number of colder, denser structures with volume filling factors ~ 0.02
to 0.12 and velocities comparable to those observed in Seyferts and LINERs, but
smaller than those observed in ULIRGs. The efficiency of the AGN wind in
transporting mass to kiloparsec distances diminishes with increasing SFR. The
mass loss rates range from 50 to 250 solar masses per year within the initial 2
Myr of evolution, which aligns with observed rates in nearby Seyferts and
ULIRGs.
