  We present a model for the Galactic supernova remnant (SNR) VRO 42.05.01,
suggesting that its intriguing morphology can be explained by a progenitor
model of a supersonically moving, mass losing star. The mass outflows of the
progenitor star were in the form of an asymmetric stellar wind focused on the
equatorial plane of the star. The systemic motion of the parent star in
combination with its asymmetric outflows excavated an extended wind bubble that
revealed a similar structure to this of VRO 42.05.01. Currently the SNR is
interacting with the wind bubble and it is dominantly shaped by it. Employing
2D hydrodynamic simulations we model VRO 42.05.01 under the framework of this
model and we reproduce its overall morphological properties. We discuss the
variations of our progenitor model in light of the current observational
uncertainties.
