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We present a numerical study of the properties of the flow produced by thecollision of a magnetized anisotropic pulsar wind with the circumbinaryenvironment. We focus on studying the impact of the high wind magnetization onthe geometrical structure of the shocked flow. This work is an extension of ourearlier studies that focused on a purely hydrodynamic interaction and weak windmagnetization. We consider the collision in the axisymmetric approximation,that is, the pulsar rotation axis is assumed to be oriented along the linebetween the pulsar and the optical star. The increase of the magnetizationresults in the expansion of the opening cone in which the shocked pulsar windpropagates. This effect is explained in the frameworks of the conventionaltheory of collimation of magnetized winds. This finding has a directimplication for scenarios that involve Doppler boosting as the primarymechanism behind the GeV flares detected with the Fermi/LAT from PSRB1259-63/LS2883. The maximum enhancement of the apparent emission is determinedby the ratio of $4\pi$ to the solid in which the shocked pulsar windpropagates. Our simulations suggest that this enhancement factor is decreasedby the impact of the magnetic field.

Modelling the interaction between relativistic and non-relativistic winds in binary pulsar systems: strong magnetization of the pulsar wind