rotate more slowly than those without winds and wind leads to enhance accretion velocities. The strong wind causes the strong accretion velocity and reduction of surface density. For the larger values of $\beta_{r,\varphi}$, a small change in $c_2$ is observed.\
Our focus is the investigate the effects of magnetic resistivity (or the Prandtl number $P_m$) and outflow on the structure of the disc. Here, the inverse of Prandtl number specifies the resistivity of the fluid as we stated in section 2. Our solutions switch back to the solution in AM12, in which the magnetic resistivity is not considered (or $P_m=\infty$). Figure 1,2,3,4 and 5 show a comparison of our model and AM12. As is clear in these Figure 1, the influence of magnetic diffusivity on the surface density and accretion velocity is more evident for deferent values of $\beta_{\phi}$. The effects of magnetic diffusion and outflow are almost the same on the structure of our model. These properties confirm the results of Faghei & Mollatayefeh (2012) and FO12.

The vertical thickness profiles are presented as a function of $\beta_{r,\varphi,z}$ for various values of exponent of $s$ in Figure 4. They show that the disc vertical thickness increases with increasing $\beta_{\phi}$, 