  The main aim of this paper is studying the effect of toroidal magnetic field
on the structure of Advection-Dominated Accretion Flows (ADAF) in the presence
of the turbulence viscosity and diffusivity due to viscosity and magnetic field
respectively. We use self-similar assumption in radial direction to solve the
magnetohydrodynamic (MHD) equations for hot accretion disk. We use spherical
coordinate $ (r, \theta, \varphi) $ to solve our equation. The toroidal
component of magnetic field is considered and all three components of the
velocity field $ \mathbf{v}\equiv (v_{r}, v_{\theta}, v_{\varphi}) $ are
present in our work. We reduce the equations to a set of differential equations
about $ \theta $ and apply the symmetric boundary condition at the equatorial
plane of the disk. Our results indicate that the outflow region, where the
redial velocity becomes positive in a certain inclination angle $ \theta_{0} $,
always exist. The results represent that the stronger the magnetic field, the
smaller the inclination angle, $ \theta_{0} $ becomes. It means that a
magnetized disk is thinner compared to a non-magnetized disk. According to the
work by \citealt{jw}, we can define three regions. The first one is called
inflow region, which starts from the disk midplane to a certain inclination $
\theta_0 $ where $ v_{r}(\theta_{0}) = 0 $. In this region, the velocity has a
negative value and the accretion material moves toward the central object. The
outflow region, where $ v_{r}(\theta) > 0 $, is placed between $ \theta_{0} $
and surface of the disk, $ \theta_{0} < \theta < \theta_{s} $. In this area,
the accretion flow moves away from the central object. The third region, which
is located between the surface of the disk and the polar axis, is called wind
region.
