  The steady-state structure of self-gravitating, magnetized accretion disks is
studied using a set of self-similar solutions which are appropriate in the
outer regions. The disk is assumed to be isothermal and the magnetic field
outside of the disk is treated in a phenomenological way. However, the internal
field is determined self-consistently. The behaviour of the solutions are
investigated by changing the input parameters of the model, i.e. mass accretion
rate, coefficients of viscosity and resistivity, and the magnetic field
configuration.
