  We investigate the properties of a hot accretion flow bathed in a poloidal
magnetic field. We consider an axisymmetric viscous resistive flow in the
steady state configuration. We assume the dominant mechanism of energy
dissipation is due to turbulence viscosity and magnetic diffusivity. A certain
fraction of that energy can be advected towards the central compact object. We
employ self-similar method in the radial direction to find a system of ODEs
with just one varible, $\theta$ in the spherical coordinates. For the existence
and maintaining of a purely poloidal magnetic in a rotating thick disk, we find
the necessary condition is a constant value of angular velocity along a
magnetic field line. We obtain an analytical solution for the poloidal magnetic
flux. We explore possible changes in the vertical structure of the disk under
the influences of even symmetric and asymmetric magnetic fields. Our results
reveal that a polar magnetic field with even symmetry about the equatorial
plane makes the disk vertically thin. Moreover, the accretion rate decreases
when we consider a strong magnetic field. Finally, we notice hot magnetized
accretion flows can be fully advected even in a slim shape.
