Colliding-wind binary systems: Diffusive shock acceleration and non-thermal emission

TL;DR

This paper models non-thermal emissions from colliding-wind binaries, incorporating diffusive shock acceleration, cosmic ray feedback, and particle cooling, to understand how emissions vary with system parameters.

Contribution

It introduces a comprehensive model including non-linear effects of cosmic ray feedback and particle cooling in colliding-wind binaries, advancing previous simplified approaches.

Findings

DSA is highly efficient without magnetic field amplification.

Non-thermal flux depends complexly on binary separation.

Inverse Compton emission varies moderately with viewing angle.

Abstract

We present a model for the non-thermal emission from a colliding-wind binary. Relativistic protons and electrons are assumed to be accelerated through diffusive shock acceleration (DSA) at the global shocks bounding the wind-wind collision region. The non-linear effects of the back-reaction due to the cosmic ray pressure on the particle acceleration process and the cooling of the non-thermal particles as they flow downstream from the shocks are included. We explore how the non-thermal particle distribution and the keV-GeV emission changes with the stellar separation and the viewing angle of the system, and with the momentum ratio of the winds. We confirm earlier findings that DSA is very efficient when magnetic field amplification is not included, leading to significantly modified shocks. We also find that the non-thermal flux scales with the binary separation in a complicated way and that the anisotropic inverse Compton emission shows only a moderate variation with viewing angle due to the spatial extent of the wind-wind collision.