Disc structure around strongly magnetic accretors: a full disc solution with buoyancy diffusivity

A full numerical solution is found for the effect of a strongly magnetic st ar on its accretion disc, for the case of magnetic buoyancy diffusion. As i n the previously considered case of turbulent diffusion, the disc becomes d isrupted when magnetic and viscous stresses become comparable. A magnetical ly induced temperature elevation leads to electron scattering opacity and r adiation pressure becoming significant far from the stellar surface, with c onsequent viscous instability and vertical disruption of the disc. This, to gether with the previous turbulent case, suggests that such a disruption me chanism owing to strongly magnetic accretors is generally operable.