  Observations indicate that wind can be generated in hot accretion flow. By
performing numerical simulations, Yuan et al. studied the detailed properties
of wind generated from weakly magnetized accretion flow. However, properties of
wind generated from strongly magnetized hot accretion flow have not been
studied. In this paper, we study the properties of wind generated from both
weakly and strongly magnetized accretion flow. We focus on how the magnetic
field strength affects the wind properties. We solve time-steady
two-dimensional magnetohydrodynamic (MHD) equations of black hole accretion in
the presence of large-scale magnetic field. We assume self-similarity in radial
direction. The magnetic field is assumed to be evenly symmetric with the
equatorial plane. We find that wind exists in both weakly and strongly
magnetized accretion flow. When magnetic field is weak (magnetic pressure is
more than 2 orders of magnitude smaller than gas pressure), wind is driven by
gas pressure gradient and centrifugal forces. When magnetic field is strong
(magnetic pressure is slightly smaller than gas pressure), wind is driven by
gas pressure gradient and magnetic pressure gradient forces. The power of wind
in strongly magnetized case is just slightly larger than that in weakly
magnetized case. The power of wind lies in a range $ P_W \sim 10^{-4}-10^{-3}
\dot M_{\rm in} c^2 $, with $ \dot M_{\rm in} $ and $ c $ being mass inflow
rate and speed of light, respectively. The possible role of wind in active
galactic nuclei feedback is briefly discussed.
