When a massive star is swung away from the stellar cluster in which it forms, a so-called runaway stellar object is produced, and its surroundings is shaped as a bow shock which can be observed. Such arc-like circumstellar nebula is the site of the star's death via a supernova explosion, and, the interaction of the supernova shock wave with its surroundings results in an asymmetric supernova remnant. We investigate the synchrotron appearance of those supernova remnants, by means of 2D magneto-hydrodynamical simulations and radiative transfer calculations of the remnant left behind a 35Mo fast-moving star. The progenitor star evolves up to the Wolf-Rayet phase and the considered space motion through the magnetised ISM is of 20 and 40km/s, respectively. The magnetic feld of the ISM has a stabilising effect regarding to the wind/ISM interface developing in the tail of the pre-supernova stellar wind bubble. Radiative transfer calculations for synchrotron radiation of our simulation models indicate that non-thermal radio emission has characteristic features accounting for the morphology of our exiled remnants of Wolf-Rayet progenitor stars. The synthetic prediction are qualitatively in accordance with the non-thermal radio appearance of several remnants from massive progenitors such as CTB109, Kes 17 and G296.5+10.0.