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Many pulsars propagate through the interstellar medium (ISM) with supersonicvelocities, and their pulsar winds interact with the interstellar medium (ISM),forming bow shocks and magnetotails (PWN). We model the propagation of pulsarsthrough the inhomogeneous ISM using non-relativistic axisymmetricmagneto-hydrodynamic (MHD) simulations. We take into account the wind from thestar, and the azimuthal and poloidal components of the magnetic field, andinvestigate the PWN at different levels of magnetization (the ratio of magneticto matter energy-densities) in the wind. We consider the interaction of PWNwith small-scale and large-scale imhomogeneities in the ISM at different valuesof magnetization. We conclude that the inhomogeneities in the ISM can changethe shapes of the bow shocks and magnetotails at different values of themagnetization.We compare the results of our simulations with the images of theGuitar Nebula and other PWN that show irregularities in the shapes of their bowshocks and magnetotails. We conclude that these irregularities may be caused bythe interaction of PWN with the inhomogeneities in the ISM.

Modelling the bow shock Pulsar Wind Nebulae propagating through a non-uniform ISM