X-ray emission and dynamics from large diameter superbubbles: The case of N 70 superbubble

TL;DR

This study uses 3D hydrodynamical simulations to analyze the morphology, dynamics, and X-ray emission of the N70 superbubble, finding that stellar winds combined with a supernova best explain observed features.

Contribution

It demonstrates that the combined effect of stellar winds and a supernova best reproduces the observed properties of N70, advancing understanding of superbubble formation.

Findings

Stellar winds plus supernova explain N70's morphology and X-ray luminosity.

Predicted interior temperatures exceed 10^8 K, but X-ray emission is faint.

Single supernova or stellar winds alone do not match observations.

Abstract

The morphology, dynamics and thermal X-ray emission of the superbubble N70 is studied by means of 3D hydrodynamical simulations, carried out with the {\sc{yguaz\'u-a}} code. We have considered different scenarios: the superbubble being the product of a single supernova remnant, of the stellar winds from an OB association, or the result of the joint action of stellar winds and a supernova event. Our results show that, in spite that all scenarios produce bubbles with the observed physical size, only those where the bubble is driven by stellar winds and a SN event are successful to explain the general morphology, dynamics and the X-ray luminosity of N70. Our models predict temperatures in excess of $10^8 \mathrm{K}$ at the interior of the superbubble, however the density is too low and the emission in thermal X-ray above $2 \mathrm{keV}$ is too faint to be detected.