  We carry out the self-similar solutions of viscous-resistive accretion flows
around a magnetized compact object. We consider an axisymmetric, rotating,
isotheral steady accretion flow which contains a poloidal magnetic field of the
central star. The dominant mechanism of energy dissipation is assumed to be the
turbulence viscosity and magnetic diffusivity due to magnetic field of the
central star. We explore the effect of viscosity on a rotating disk in the
presence of constant magnetic diffusivity. We show that the dynamical
quantities of ADAFs are sensitive to the advection and viscosity parameters.
Increase of the $\alpha$ coefficient in the $\alpha$-prescription model
decreases the radial velocity and increases the density of the flow. It also
affects the poloidal magnetic field considerably.
