X-ray emission from interacting massive binaries: a review of 15 years of progress

TL;DR

This review summarizes 15 years of progress in understanding X-ray emissions from interacting massive binaries, emphasizing advances from new observatories and future research prospects.

Contribution

It provides a comprehensive overview of theoretical and observational developments in X-ray emissions from massive binaries over the past 15 years.

Findings

Enhanced understanding of shock-heated plasma in wind-wind interactions

Detailed observational data from current X-ray observatories

Future prospects with next-generation X-ray satellites

Abstract

Previous generations of X-ray observatories revealed a group of massive binaries that were relatively bright X-ray emitters. This was attributed to emission of shock-heated plasma in the wind-wind interaction zone located between the stars. With the advent of the current generation of X-ray observatories, the phenomenon could be studied in much more detail. In this review, we highlight the progress that has been achieved in our understanding of the phenomenon over the last 15 years, both on theoretical and observational grounds. All these studies have paved the way for future investigations using the next generation of X-ray satellites that will provide crucial information on the X-ray emission formed in the innermost part of the wind-wind interaction.