We present the effect of a hydrodynamical wind on the structure and the surface temperature of a vertically self-gravitating magnetized advection-dominated accretion flows (ADAFs) using self-similar solutions. Also a model for an axisymmetric, steady-state, vertically selfgravitating hot accretion flow threaded by a toroidal magnetic field has been formulated. The model is based on α-prescription for turbulence viscosity. It is found that the thickness and radial velocity of the disc are reduced significantly as wind gets stronger. In particular, the solutions indicated that the wind and advection have the same effects on the structure of the disc. We also find that the thin ADAF becomes hotter by including the wind parameter and the self-gravity parameter.

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