Modelling the synchrotron emission from O-star colliding wind binaries

TL;DR

This paper models the synchrotron emission from O-star colliding wind binaries, focusing on the non-thermal radio variability caused by relativistic electrons accelerated in wind collision shocks.

Contribution

It introduces a new model for simulating non-thermal synchrotron emission in O-star binary systems, specifically applied to Cyg OB2 No.9.

Findings

Preliminary modeling results of Cyg OB2 No.9's colliding winds.

Insights into the origin of radio variability in O-star binaries.

Foundation for future detailed emission studies.

Abstract

Many early-type stars are in binary systems. A number of them shows radio emissivity with periodic variability. This variability is associated with non-thermal synchrotron radiation emitted by relativistic electrons. The strong shocks necessary to accelerate the electrons up to high energies are produced by the collision of the radiatively-driven stellar winds. A study of the non-thermal emission is necessary in order to investigate O-star colliding wind binaries. Here preliminary results of our modeling of the colliding winds in Cyg OB2 No.9 are presented.