  Core-collapse supernova remnants are structures of the interstellar medium
(ISM) left behind the explosive death of most massive stars (smaller or equal
to 40 Mo). Since they result in the expansion of the supernova shock wave into
the gaseous environment shaped by the star wind history, their morphology
constitutes an insight into the past evolution of their progenitor star.
Particularly, fast-moving massive stars can produce asymmetric core-collapse
supernova remnants. We investigate the mixing of materials in core-collapse
supernova remnants generated by a moving massive 35 Mo star, in a magnetised
ISM. Stellar rotation and the wind magnetic field are time-dependently included
into the models which follow the entire evolution of the stellar surroundings
from the zero age main sequence to 80 kyr after the supernova explosion. It is
found that very little main sequence material is present in remnants from
moving stars, that the Wolf-Rayet wind mixes very efficiently within the 10 kyr
after the explosion, while the red supergiant material is still unmixed by 30
per cent within 50 kyr after the supernova. Our results indicate that the
faster the stellar motion, the more complex the internal organisation of the
supernova remnant and the more effective the mixing of ejecta therein. In
contrast, the mixing of stellar wind material is only weakly affected by
progenitor motion, if at all.
