and have a flattened time-averaged radial density profile, $\rho\propto r^{-\frac{1}{2}}$, where much flatter than usual ADAFs with $\rho\propto r^{-\frac{3}{2}}$. In CDAFs the most part of the energy which realized in inner most region of accretion flow is transport outward by convection.

Mass loss mechanism (in the form of wind or outflow) is an interesting phenomenon in the structure and evolution of the accretion discs. The existence of wind and outflow has been observationally verified in various astronomical objects like AGNs and YSOs (Whelan et al. 2005, Bally et al. 2007). **On the other hand several numerical simulation have been performed and they clearly confirm the existence of outflow in such systems (Yuan et al. (2012a, 2012b), Narayan et al. (2012), Li, Ostriker & Sunyaev (2013), Yuan et al. (2015), Bu et al. (2016a, 2016b).** In these objects some part of angular momentum of the accretion flow will dissipated outward in the form of wind and jet. For generating outflow various driving forces are proposed, such as thermal, radiative and magnetic field. The wind mechanism has been investigated by many others (Meier 1979, Fukue 1989, Abbassi et al. 2008, 2010, Ghasemnezhad & Abbassi 2016). The effect of magnetic field on the 