Density slices for cluster I (R_c = 0.6 pc, top) and cluster III (R_c = 1 pc, bottom). The inner ±8 pc are shown, which excludes the superbubble shell. In the left-most panels (a and e), all stars are on the main sequence. The cluster wind is in a quasi-stationary state, slowly expanding over time but not changing geometry. At t > 200 kyr (panels b–d and f–h), the most massive stars consecutively evolve into WR stars. The flow rearranges into a new quasi-stationary state within ~20 kyr after each new WR wind (see panels b–c and e–f). The wind termination shock has a complex, non-spherical geometry, which appears different in different slices (see panels g–h). The white circle in panels g–h indicates the shock radius predicted by 1D analytical theory (Weaver et al. 1977).