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A very small fraction of (runaway) massive stars have masses exceeding$60$-$70\, \rm M_{\odot}$ and are predicted to evolve as Luminous-Blue-Variableand Wolf-Rayet stars before ending their lives as core-collapse supernovae. Our2D axisymmetric hydrodynamical simulations explore how a fast wind ($2000\, \rmkm\, \rm s^{-1}$) and high mass-loss rate ($10^{-5}\, \rm M_{\odot}\, \rmyr^{-1}$) can impact the morphology of the circumstellar medium. It is shapedas 100 pc-scale wind nebula which can be pierced by the driving star when itsupersonically moves with velocity $20$-$40\, \rm km\, \rm s^{-1}$ through theinterstellar medium (ISM) in the Galactic plane. The motion of such runawaystars displaces the position of the supernova explosion out of their bow shocknebula, imposing asymmetries to the eventual shock wave expansion andengendering Cygnus-loop-like supernova remnants. We conclude that the size (upto more than $200\, \rm pc$) of the filamentary wind cavity in which thechemically enriched supernova ejecta expand, mixing efficiently the wind andISM materials by at least $10\%$ in number density, can be used as a tracer ofthe runaway nature of the very massive progenitors of such $0.1\, \rm Myr$ oldremnants. Our results motivate further observational campaigns devoted to thebow shock of the very massive stars BD+43 3654 and to the close surroundings ofthe synchrotron-emitting Wolf-Rayet shell G2.4+1.4.

Wind nebulae and supernova remnants of very massive stars