Abstract Accretion disk winds can leave from active galactic nuclei (AGNs) and interact with the interstellar medium (ISM) of their host galaxies. We perform two-dimensional numerical simulations to investigate the interaction of AGNs winds and ISM. We study the properties of outflows in the 1 − 1000pc region under different gravitational potentials and ISM gas densities, and compare these ionized outflows with the observed warm absorbers (WAs). We find that AGNs winds drag the ISM and transfer their momentum/energy to the ISM. The properties of winds depend on the gas density of the initial ISM. The higher the initial ISM density, the lower the winds speed, and the narrower the opening angle of the winds. For the case of ρ0 = 10−25gcm−3, the winds have the strongest intensity at the outer boundary. They can blow the ISM gas, giving feedback on star formation and galaxy evolution. We also find that the interaction of AGNs winds and ISM can generate WAs in certain conditions and AGNs winds play some roles in generating WAs.