Gas density (left) and magnetic field strength along cuts through the 2D simulation results at the end of stellar evolution (far-right panels of Figs. 3, 6, B.2, and B.4). Each cut starts at the central star and moves either along the R-axis (dashed lines) or at a 45^o angle (continuous lines) between the R- and Z-axes. The compression of the outer shell decreases with increasing field strength, Alfvén-waves weakening the shock.