The initial mass function predicts that very few massive stars can have a zero-age-main-
sequence mass exceeding 60Mo. These rare objects can evolve to exotic phases of stellar
evolution, such as the Luminous-Blue-Variable and Wolf-Rayet phases, and might finish
their lives via a core-collapse supernova explosion. We present 2D axisymmetric hydro-
dynamical simulations of the surroundings of such very massive stars, characterised by
both a high mass-loss rate and by strong wind velocities. We found that it is shaped as
a 100 pc large stellar wind bubble. In the context of a fast-moving stellar motion of the
order of about 20-40km/s, into the warm phase of the interstellar medium (ISM), these
stars can escape their own circumstellar bubble. The location of the supernova explosion,
where the star dies, is therefore off-set to the geometrical center of its pre-supernova cir-
cumstellar nebula, and, as a consequence, the subsequent supernova remnant rejects the
asymmetries of the shaped medium. We find that the formed, distorted, cavity of stellar
wind in which the enriched supernova ejecta expand hosts an effcient mixing of stellar
wind and ISM materials. We propose that peculiar enrichment of the ISM can be used
as a tracer of the runaway nature of the high-mass stellar progenitors of these supernova
remnants.