3D numerical model of the Omega Nebula (M17): simulated thermal X-ray emission

TL;DR

This paper presents 3D hydrodynamical simulations of the Omega Nebula's superbubble, modeling stellar winds and comparing synthetic X-ray emissions with observations, successfully reproducing observed morphology and luminosity.

Contribution

The study introduces detailed 3D models of M17's superbubble considering individual stellar winds and compares synthetic X-ray emissions with observations, without including thermal conduction effects.

Findings

Models match observed X-ray morphology.

Simulated X-ray luminosity agrees with ROSAT data.

Thermal conduction effects are not necessary for accurate modeling.

Abstract

We present 3D hydrodynamical simulations of the superbubble M17, also known as the Omega nebula, carried out with the adaptive grid code yguazu'-a, which includes radiative cooling. The superbubble is modelled considering the winds of 11 individual stars from the open cluster inside the nebula (NGC 6618), for which there are estimates of the mass loss rates and terminal velocities based on their spectral types. These stars are located inside a dense interstellar medium, and they are bounded by two dense molecular clouds. We carried out three numerical models of this scenario, considering different line of sight positions of the stars (the position in the plane of the sky is known, thus fixed). Synthetic thermal X-ray emission maps are calculated from the numerical models and compared with ROSAT observations of this astrophysical object. Our models reproduce successfully both the observed X-ray morphology and the total X-ray luminosity, without taking into account thermal conduction effects.