Wind nebulae and supernova remnants of very massive stars
  A very small fraction of (runaway) massive stars have masses exceeding
$60$-$70\, \rm M_{\odot}$ and are predicted to evolve as Luminous-Blue-Variable
and Wolf-Rayet stars before ending their lives as core-collapse supernovae. Our
2D axisymmetric hydrodynamical simulations explore how a fast wind ($2000\, \rm
km\, \rm s^{-1}$) and high mass-loss rate ($10^{-5}\, \rm M_{\odot}\, \rm
yr^{-1}$) can impact the morphology of the circumstellar medium. It is shaped
as 100 pc-scale wind nebula which can be pierced by the driving star when it
supersonically moves with velocity $20$-$40\, \rm km\, \rm s^{-1}$ through the
interstellar medium (ISM) in the Galactic plane. The motion of such runaway
stars displaces the position of the supernova explosion out of their bow shock
nebula, imposing asymmetries to the eventual shock wave expansion and
engendering Cygnus-loop-like supernova remnants. We conclude that the size (up
to more than $200\, \rm pc$) of the filamentary wind cavity in which the
chemically enriched supernova ejecta expand, mixing efficiently the wind and
ISM materials by at least $10\%$ in number density, can be used as a tracer of
the runaway nature of the very massive progenitors of such $0.1\, \rm Myr$ old
remnants. Our results motivate further observational campaigns devoted to the
bow shock of the very massive stars BD+43 3654 and to the close surroundings of
the synchrotron-emitting Wolf-Rayet shell G2.4+1.4.
