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Observations indicate that wind can be generated in hot accretion flow. Byperforming numerical simulations, Yuan et al. studied the detailed propertiesof wind generated from weakly magnetized accretion flow. However, properties ofwind generated from strongly magnetized hot accretion flow have not beenstudied. In this paper, we study the properties of wind generated from bothweakly and strongly magnetized accretion flow. We focus on how the magneticfield strength affects the wind properties. We solve time-steadytwo-dimensional magnetohydrodynamic (MHD) equations of black hole accretion inthe presence of large-scale magnetic field. We assume self-similarity in radialdirection. The magnetic field is assumed to be evenly symmetric with theequatorial plane. We find that wind exists in both weakly and stronglymagnetized accretion flow. When magnetic field is weak (magnetic pressure ismore than 2 orders of magnitude smaller than gas pressure), wind is driven bygas pressure gradient and centrifugal forces. When magnetic field is strong(magnetic pressure is slightly smaller than gas pressure), wind is driven bygas pressure gradient and magnetic pressure gradient forces. The power of windin strongly magnetized case is just slightly larger than that in weaklymagnetized 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 inflowrate and speed of light, respectively. The possible role of wind in activegalactic nuclei feedback is briefly discussed.

The Effects of Magnetic Field Strength on Properties of Wind Generated from Hot Accretion Flow