Magnetohydrodynamic processes in thin accretion disks involving magnetic viscosity are investigated. The relevant MHD equations for the thin disk approximation and the anomalous magnetic viscosity dependent on temperature $T$ and radius $r$ are included. These stationary structures, including distributions of the surface mass density, temperature, in-flow velocity and magnetic fields of a disk around a young stellar object, are numerically examined. It is shown that the consideration of anomalous viscosity is necessary for the validity of the distributions. For example, the surface density is a decreasing function of radius because of it and there is a strange increasing part in the distribution of the density if it is ignored. In particular the distribution of effective temperature is a smoothly decreasing function of radius with power index $q\,{=}\,{-}\frac{1}{2}$, corresponding to the observed radiation flux density, provided that the magnetic fields are suitably chosen.