we was stated as: $$\nu=P_{m}\eta=\alpha c_{s} H$$ where $P_{m}$ is the magnetic Prandt number of the turbulence, which adopted to be a constant less than unity, $\eta$ is the magnetic diffusivity (Shadmehri 2004). The last term on the right hand side of the energy equation represents the energy loss due to wind or outflow (Knigge 1999). In our model $\zeta$ is a free and dimensionless parameter. The large $\zeta$ corresponds to more energy extraction from the disc because of wind (Knigge 1999).

Finally since we consider three components of magnetic field, the three components of induction equation can be written as: $$\dot{B}_{r}=0$$

$$\dot{B}_{\varphi}=\frac{d}{dr}[V_\varphi B_r - V_r B_\varphi+\frac{\eta}{r}\frac{d}{dr}(r B_\varphi)]$$

$$\dot{B}_{z}=-\frac{d}{dr}[rV_r B_z -\eta r\frac{d B_z}{dr}]$$

where $\dot{B}_ r,\varphi,z$ is the field escaping/creating rate due to magnetic instability or dynamo effect. Now we have a set of MHD equations that control the structure of magnetized CDAFs. The solutions of these coupled equation are strongly correlated to given values of viscosity, connectivity, magnetic field strength, $\beta_{r, \phi, z}$ and degree of advection $f$. In the next section we will demonstrate the self-similar solution of this MHD equations.

Self-Similar Solutions
======================

The basic equations of our models was discussed in the last section. We use 