VRO 42.05.01: A supernova remnant resulted by a supersonic, mass losing progenitor star

TL;DR

This paper models the supernova remnant VRO 42.05.01 as resulting from a supersonic, mass-losing star whose asymmetric stellar wind and motion created a wind bubble, shaping the remnant's morphology, supported by hydrodynamic simulations.

Contribution

It introduces a novel progenitor model involving asymmetric stellar winds and star motion to explain VRO 42.05.01's morphology, validated through hydrodynamic simulations.

Findings

Hydrodynamic simulations successfully reproduce the remnant's morphology.

The asymmetric wind and star motion explain the observed structure.

The model aligns with current observational data.

Abstract

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.