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We perform two-dimensional simulations to study how the wind strength changeswith accretion rate. We take into account bremsstrahlung, synchrotron radiationand the Comptonization. We find that when the accretion rate is low, radiativecooling is not important, the accretion flow is hot accretion flow. For the hotaccretion flow, wind is very strong. The mass flux of wind can be $\sim 50\%$of the mass inflow rate. When the accretion rate increases to a value at whichradiative cooling rate is roughly equal to or slightly larger than viscousheating rate, cold clumps can form around the equatorial plane. In this case,the gas pressure gradient force is small and wind is very weak. Our results maybe useful for the sub-grid model of active galactic nuclear feedback study.

On the wind production from hot accretion flows with different accretion rates