(2001), we employ the Schawrzchild units for the radius, i.e., $R=\frac{r}{R_s}$ and $R_{out}=\frac{r_{out}}{R_s}$. $R_s=\frac{2GM_{\ast}}{c^{2}}=2.95 \times 10^{5} m \  cm$ is the Schawrzchild radius and $c$ and $m$ are light speed and the black hole mass in solar units $(=\frac{M_{\ast}}{M_{\odot}})$ respectively. So we can write the density as: $$\rho=\frac{c_0}{c_4}\rho_{out} R^{\frac{3}{2}-s}_{out} (R)^{s-\frac{3}{2}}=\frac{c_0}{c_4}\rho_0 (R)^{s-\frac{3}{2}}$$ where $\rho_{0}=\rho_{out} R^{\frac{3}{2}-s}_{out}$. As we stated in introduction, for $s=1$ the ADAF(+wind+convection) solutions include of CDAF models.

In this model, we can estimate the temperature of the dics as (Akizuki & Fukue 2006): $$\frac{\Re}{\bar{\mu}}T=c_\mathrm{s}^{2}=c_3\frac{GM_{\star}}{r}$$ where $\Re$ the gas constant and $\bar{\mu}$ the mean molecular weight ($\bar{\mu}=0.5$). So, $$T=c_3\frac{c^{2}\bar{\mu}}{2 \Re}(\frac{r}{R_\mathrm{s}})^{-1}=2.706 \times10^{12}c_3(\frac{r}{R_\mathrm{s}})^{-1}$$ $$=2.706 \times10^{12}c_3(R)^{-1}=T_0 c_3 (R)^{-1}$$ In this formula the coefficient $c_3$ implicitly depends on the wind, magnetic diffusion, magnetic field, advection and viscosity parameters, ($s, \eta (or P_m), \beta_{r,\varphi,z}, f, \alpha$). Total emissivity due the bremsstrahlung emission is (Rybicki & Lightman 1986): $$q_{bremss}(T,\nu)=2.4\times 10^{10} T^{-\frac{1}{2}}\rho^{2}\exp(\frac{-h\nu}{KT}) G_b$$ $$(erg s^{-1} cm^{-3}Hz^{-1})$$ where $G_b$, $K$ and $h$ are the Gaunt factor (and is around $1$), the Boltzmann constant and Planck’s constant respectively. We have ignored a weak frequency-dependent Gaunt factor. As we see the density $\rho$ instead of temperature is the dominant factor in bremsstrahlung emission. As the above equation, the bremsstrahlung emission 