outflow and global magnetic field. Faghei & Omidvand (2012, hear after FO12) studied radial self similar solution of accretion flow in the presence of toroidal magnetic field, convection and resistivity. They ignored the effect of outflow and global magnetic field. AM12 studied the self similar solution of CDAFs with a global magnetic field and outflow. We have improved AM12 paper by adding the magnetic resistivity parameter and then have compared two solutions.

The main aim of our present work is highlighting observational consequences of CDAF models, focusing in particular on power spectra. Our results are similar to those of Blandford & Begelman(1999), AM12 who have assumed that a significant fraction of mass in an ADAF would be lost to outflow/wind, rather than accreting onto central object. In ADAFs the importance of outflows can be shown by a radial density profile as ($\rho \propto r^{s-\frac{3}{2}}$) which $(0<s<1)$. The density profile in CDAFs is equivalent to $s=1$ ($\rho \propto r^{-\frac{1}{2}}$). In order to capture many feature of CDAFs we have considered various values of $s$ in this study.

In CDAFs the convection motions transport a luminosity $L_{c}\approx (10^{-3}-10^{-2})\dot{M} c^{2}$ from small to large radii. The most of the energy that transport outward 