  We model the vertical structure of magnetized accretion disks subject to
viscous and resistive heating, and irradiation by the central star. We apply
our formalism to the radial structure of magnetized accretion disks threaded by
a poloidal magnetic field dragged during the process of star formation
developed by Shu and coworkers. We consider disks around low mass protostars, T
Tauri, and FU Orionis stars. We consider two levels of disk magnetization,
$\lambda_{sys} = 4$ (strongly magnetized disks), and $\lambda_{sys} = 12$
(weakly magnetized disks). The rotation rates of strongly magnetized disks have
large deviations from Keplerian rotation. In these models, resistive heating
dominates the thermal structure for the FU Ori disk. The T Tauri disk is very
thin and cold because it is strongly compressed by magnetic pressure; it may be
too thin compared with observations. Instead, in the weakly magnetized disks,
rotation velocities are close to Keplerian, and resistive heating is always
less than 7\% of the viscous heating. In these models, the T Tauri disk has a
larger aspect ratio, consistent with that inferred from observations. All the
disks have spatially extended hot atmospheres where the irradiation flux is
absorbed, although most of the mass ($\sim 90-95$ \%) is in the disk midplane.
With the advent of ALMA one expects direct measurements of magnetic fields and
their morphology at disk scales. It will then be possible to determine the
mass-to-flux ratio of magnetized accretion disks around young stars, an
essential parameter for their structure and evolution. Our models contribute to
the understanding of the vertical structure and emission of these disks.
