Magnetic models of accretion discs are presented and discussed. The magnetic field is generated and maintained in the disc by a dynamo mechanism. The relative magnitudes of the azimuthal viscous and magnetic forces depend on the diffusion mechanism considered. With buoyancy dominant, magnetic stresses control the radial advection of angular momentum. With buoyancy and turbulent diffusion, viscous and magnetic advection of angular momentum become comparable. All the magnetic disc solutions have eigenstate structures, corresponding to differing vertical variations of the field.