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We present high resolution simulations with RAMSES of supersonic collidingstellar winds. The collision results in a double shock structure which issubject to different instabilities. The Kelvin-Helmholtz instability (KHI)introduces some mixing and variability. For isothermal winds, the Non-linearThin Shell Instability violently affects the interaction region. Properlymodelling these instabilities requires a high enough resolution and an adaptednumerical method, especially when one of the winds strongly dominates the otherone. At large scale, orbital motion is expected to turn the shocked zone into aspiral but we find that in some configurations the KHI may disrupt the spiral.A colliding wind structure is also expected in gamma-ray binaries composed of amassive star and a young pulsar which emits a highly relativistic wind.Numerical simulations are necessary to understand the geometry of such systemsand should take into account the relativistic nature of the pulsar wind. Weimplemented a second order Godunov method to solve the equations ofrelativistic hydrodynamics with RAMSES, including the possibility for AdaptiveMesh Refinement. After a brief overview of our numerical implementation, wewill present preliminary simulation that contrast the structure of the flow ingamma-ray and stellar binaries.

Modelling colliding wind binaries with RAMSES, extension to special relativity