The Outer Shock of the Oxygen-Rich Supernova Remnant G292.0+1.8: Evidence for the Interaction with the Stellar Winds from its Massive Progenitor

TL;DR

This study uses deep X-ray observations to analyze the outer shock of supernova remnant G292.0+1.8, revealing interaction with a dense stellar wind from its massive progenitor star, consistent with a red supergiant wind model.

Contribution

It provides detailed measurements of the shock structure and ambient density profile, supporting the interaction with a stellar wind rather than a uniform interstellar medium.

Findings

Outer shock propagates into a medium with decreasing density

Ambient density matches a red supergiant wind profile

Estimated wind mass is 15-40 solar masses

Abstract

We study the outer-shock structure of the oxygen-rich supernova remnant G292.0+1.8, using a deep observation with the Chandra X-ray Observatory. We measure radial variations of the electron temperature and emission measure that we identify as the outer shock propagating into a medium with a radially decreasing density profile. The inferred ambient density structure is consistent with models for the circumstellar wind of a massive progenitor star rather than for a uniform interstellar medium. The estimated wind density n_H = 0.1 ~ 0.3 cm^-3) at the current outer radius (~7.7 pc) of the remnant is consistent with a slow wind from a red supergiant (RSG) star. The total mass of the wind is estimated to be ~ 15 - 40 solar mass (depending on the estimated density range), assuming that the wind extended down to near the surface of the progenitor. The overall kinematics of G292.0+1.8 are consistent with the remnant expanding through the RSG wind.