Animation A_wind, shows the evolution of the circumstellar bubble according to simulation A (no interstellar magnetic field) for the pre-supernova phase. (The animation is available online.)

Animation B_wind shows the pre-supernova evolution of the circumstellar bubble according to simulation B (B_ISM = 5 μG). (The animation is available online.)

Animation A_sn shows the expansion of the supernova remnant for simulation A. (The animation is available online.)

Animation B_sn shows the expansion of the supernova remnant for simulation B. (The animation is available online.)

Animation C_wind shows the pre-supernova evolution of the circumstellar bubble according to simulation C (B_ISM = 10 μG). (The animation is available online.)

Animation C_sn shows the expansion of the supernova remnant for simulation C. (The animation is available online.)

Animation D_wind shows the pre-supernova evolution of the circumstellar bubble according to simulation D (B_ISM = 20 μG). (The animation is available online.)

Animation D_sn shows the expansion of the supernova remnant for simulation D. (The animation is available online.)

Animation E_wind shows the pre-supernova evolution of the circumstellar bubble according to simulation E (B_ISM = 5 μG, low density warm ISM). (The animation is available online.)

Animation E_sn shows the expansion of the supernova remnant for simulation E. (The animation is available online.)

Animation F_wind shows the pre-supernova evolution of the circumstellar bubble according to simulation F (B_ISM = 5 μG, high density warm ISM). (The animation is available online.)

Animation F_sn shows the expansion of the supernova remnant for simulation F. (The animation is available online.)

Similar to Figs. 2 and 5 but for Simulation C with an external magnetic field of 10 μG. This plot shows both the logarithm of the density in [cgs] and the magnetic field lines. The scale of the central and right panels in this figure is 80 × 80 pc. As for simulation B, the swept-up shell of shocked ISM is relatively thick, which prevents the formation of thin-shell instabilities; and the contact discontinuity between shocked wind and swept-up ISM is strongly asymmetric. Although the RSG shell can form freely against the spherically symmetric wind termination shock (right side of centre panel), the expanding WR nebula is strongly affected by the asymmetry of the bubble (left side of right panel).

Similar to Figs. 3 and 6 but for simulation C with an external magnetic field of 10 μG. Because the supernova expansion is spherical and the outer boundary of the bubble is strongly ellipsoid, the supernova will first collide with the outer shell at the “waist” of the bubble, noticeable on the left side of the right panel. In fact, on the right side of the right panel, the supernova is already moving back toward the centre in the perpendicular direction, whereas it is still expanding in the direction parallel to the field.

Similar to Figs. 2, 5 and B.1, but for simulation D, which has a 20 μG  interstellar magnetic field The shocked wind bubble is highly asymmetric from the earliest stages of the evolution and stops expanding in the direction perpendicular to the magnetic field after it reaches approximately 7 pc. The elongated shape of the bubble strongly influences the development of the WR nebula (right panel).

Similar to Figs. 3, 6, and B.2 but for simulation D with an external magnetic field of 20 μG. The scale of each panel is 120 × 120 pc. The strongly asymmetrical shape of the bubble causes the supernova to expand along the z-axis after recoiling from the outer edge.

Shape of the bubble for simulation F after 3, 3.5, 3.75, and 4 Myr. The tips of the bubble are squeezed off by the magnetic field. This effect is enhanced by the 2D nature of our simulations and may not actually occur in 3D.