paper). As the wind becomes stronger, the inner mass accretion rate $\dot{m}_{in}(=\frac{\dot{M}_{in}}{\dot{M}_{Edd}} = \dot{m}_{out} R_{out}^{-s})$ becomes smaller than $\dot{m}_{out}$, so the importance of bermesstrahlung emission increases. So by adding the wind parameter $(s)$ the maximum of bermesstrahlung luminosity increases. Quataert & Narayan (1999) stated the bremsstrahlung emission produces a peak that extends from a few to a few hundred $kev$. Also we have shown that the peak of power spectrum is located approximately at $ h\nu \approx 41 keV $, which is independent of the strength of winds in the system. This result is in full agreement with perviously study by Quataert & Narayan (1999).

Also, we are plotted the radiation spectrum of CDAFs for different values of all components of magnetic field. The effect of toroidal magnetic field on the radiation spectrum is similar to wind parameter. While the effect of $\beta_{z}$ and $p_m$ on the power spectrum are almost negligible.

Summary and Conclusion
======================

The CDAFs model consistently explain radiation inefficient accretion flow (RIAF) in the presence of convection. Many authors studied the importance of convection in RIAFs (CDAFs model) by means of numerical simulation or even analytically using the mixing length theory. Also observational results and MHD 