accretion rate and define as: $$\dot{m}=\frac{\dot{M}_\mathrm{out}}{\pi \Sigma_{out} r_{out}\sqrt{\frac{GM_{\ast}}{r_{out}}}}$$ Also, the field scaping/creating rate $\dot{B}_r,\varphi,z$ is written as follows: $$\dot{B}_{r,\varphi,z}=\dot{B}_{0 r,0\varphi,z}(\frac{r}{r_{out}})^{\frac{s}{2}-\frac{11}{4}}$$ By using of the self similarity solutions, we will have: $$\dot{B}_{r}=0$$ $$\dot{B}_{0\varphi}=\frac{1}{2}(s-\frac{7}{2})\frac{GM_{\ast}}{r^{\frac{5}{2}}_{out}}\sqrt{\frac{4\pi c_0 c_3 \Sigma_{out}}{c_4}}[c_2\sqrt{B_r}+c_1\sqrt{B_\varphi}$$ $$-(s-\frac{1}{2})\frac{\alpha c_4 \sqrt{c_3}}{2 P_m}]$$

$$\dot{B}_{0z}=\frac{1}{2}(s-\frac{3}{2})\frac{GM_{\ast}}{r^{\frac{5}{2}}_{out}}\sqrt{\frac{4\pi c_0 c_3 \Sigma_{out}}{c_4}}[c_1
 -(s-\frac{5}{2})\frac{\alpha c_4 \sqrt{c_3}}{2 P_m}]$$

We can solve these equations numerically. The equations reduce to the equations of AM12 without the resistivity parameter $\eta=0$ or ($P_m=\infty$), . Also our equations reduce to the result of FO12 without outflow/wind parameter, radial and vertical magnetic filed.

The radiation properties of CDAFs
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Using self-similar solutions obtained in the pervious section we will able to produce observational appearance of CDAFs. The inner part of accretion discs, where ADAFs or CDAFs conditions is valid, has a very high temperature and is moreover optically thin and magnetized. The relevant radiation processes are synchrotron emission, bremesstrahlung and modified Comptonization. Bremsstrahlung emission is the main cooling process for high temperature $T (>10^{7} K)$ plasma. In this paper, we have supposed that the bremsstrahlung radiation is the only contributor to our spectrum model.\
As we have shown in the last section, the density of gas in our model is : $$\rho=\frac{c_0}{c_4}(\frac{1}{2}\frac{\Sigma_{out}}{r_{out}})(\frac{r}{r_{out}})^{s-\frac{3}{2}}=\frac{c_0}{c_4}\rho_{out} (\frac{r}{r_{out}})^{s-\frac{3}{2}}$$

Following $Ball$ et al. 