top left In Figure 6. In the top right panel and bottom left panel we show that surface temperature increases by increasing toroidal and vertical magnetic field parameters. But the effect of $\beta_{\varphi}$ is more evident. And finally in the bottom right panel we can see the values of magnetic resistivity don’t affect the surface temperature. So the disc is hotter with strong wind or even stronger magnetic field.

The radiation spectrum of the hot CDAF around a $10^{8} M_{\odot}$ black hole is represented in Figure 7 for several values of wind, radial and vertical magnetic field and resistivity parameters. The corresponding values of $\dot{m}(=\frac{\dot{M}}{\dot{M}_{Edd}})$ and $R_{out}$ are $10^{-3.9}$ and $10^{3}$ respectively. Luminosity depends explicitly on some of our input parameters like $s$, $R_{out}$, $m$, $c_4$ ( see equation 60) and implicitly on other parameters. The bremsstrahlung X-ray emission has been adopted since it is dominant mechanism in the outer parts of CDAFs.

As can be seen in figure 7, the maximum of $\nu L_{\nu}$ is highly depends on the given values of wind parameter. Whenever bremsstrahlung emission dominants, the X-ray emission depends directly on $\dot{m}_{out}(=\frac{\dot{M}_{out}}{\dot{M}_{Edd}})$ (see section 3.1 in Quataert & Narayan 1999 and see equation 57 in our 