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Non-thermal emission has been detected in WR-stars for many years at longwavelengths spectral range, in general attributed to synchrotron emission. Twokey ingredients are needed to explain such emissions, namely magnetic fieldsand relativistic particles. Particles can be accelerated to relativistic speedsby Fermi processes at strong shocks. Therefore, strong synchrotron emission isusually attributed to WR binarity. The magnetic field may also be amplified atshocks, however the actual picture of the magnetic field geometry, intensity,and its role on the acceleration of particles at WR binary systems is stillunclear. In this work we discuss the recent developments in MHD modelling ofwind-wind collision regions by means of numerical simulations, and the coupledparticle acceleration processes related.

Magnetic fields, non-thermal radiation and particle acceleration in colliding winds of WR-O stars