Magnetic interchange instability in the strong field case (μ = 2) for the GDSPH simulation with 50³ resolution. Left panel: zoom-in of the disc structure seen face-on in Fig. 11 and right panel: same region at a later time. The white arrows show the direction of velocity and the colour scale indicates density. The instability launches magnetized bubbles in the azimuthal direction. At later times we can see that the central star starts to accrete again along the filamentary structure. These figures can be compared to the results from Krasnopolsky et al. (2012).