A class of self-gravitating, magnetized accretion disks

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