  The dynamics of colliding wind binary systems and conditions for efficient
particle acceleration therein have attracted multiple numerical studies in the
recent years. These numerical models seek an explanation of the thermal and
non-thermal emission of these systems as seen by observations. In the
non-thermal regime, radio and X-ray emission is observed for several of these
colliding-wind binaries, while gamma-ray emission has so far only been found in
$\eta$ Carinae and possibly in WR 11. Energetic electrons are deemed
responsible for a large fraction of the observed high-energy photons in these
systems. Only in the gamma-ray regime there might be, depending on the
properties of the stars, a significant contribution of emission from neutral
pion decay. Thus, studying the emission from colliding-wind binaries requires
detailed models of the acceleration and propagation of energetic electrons.
This in turn requires a detailed understanding of the magnetic field, which
will not only affect the energy losses of the electrons but in case of
synchrotron emission also the directional dependence of the emissivity. In this
study we investigate magnetohydrodynamic simulations of different colliding
wind binary systems with magnetic fields that are strong enough to have a
significant effect on the winds. Such strong fields require a detailed
treatment of the near-star wind acceleration zone. We show the implementation
of such simulations and discuss results that demonstrate the effect of the
magnetic field on the structure of the wind collision region.
