by convection can be radiated from the outer regions of the flow as thermal bremsstrahlung emission which is a function of temperature and density of accreting gas (Igumenshchev, & Abramowicz (2000) , Ball et al. 2001). We assumed the same mechanism in our study.

This paper organized as follows. The basic equations and assumptions are presented in section 2. Self-similar solutions are presented in section 3. The radiation properties of CDAFs are discussed in section 4. We show the result in section 5 and finally we present the summary and conclusion in section 6.

The Basic Equations
===================

We use the cylindrical coordinates $(r, \varphi, z)$ to write the MHD equations of steady state and axi-symmetric ($\frac{\partial}{\partial
\phi}=\frac{\partial}{\partial t}=0$) hot accretion flow around compact black hole of mass $M_{\star}$. Following AM12, we assume a magnetic field with three components $(B_{r}, B_{\varphi},
B_{z})$. We have vertically integrated the equations and then all our physical variables become only a function of radial distances, $r$. Moreover, the disc suppose to have Newtonian gravity in radial direction and also we neglect the self-gravity of the discs and the general relativistic effects. The disc is supposed to turbulent and possesses an effective turbulent viscosity. We 