  We perform two-dimensional simulations to study how the wind strength changes
with accretion rate. We take into account bremsstrahlung, synchrotron radiation
and the Comptonization. We find that when the accretion rate is low, radiative
cooling is not important, the accretion flow is hot accretion flow. For the hot
accretion 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 which
radiative cooling rate is roughly equal to or slightly larger than viscous
heating 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 may
be useful for the sub-grid model of active galactic nuclear feedback study.
