  Many pulsars propagate through the interstellar medium (ISM) with supersonic
velocities, and their pulsar winds interact with the interstellar medium (ISM),
forming bow shocks and magnetotails (PWN). We model the propagation of pulsars
through the inhomogeneous ISM using non-relativistic axisymmetric
magneto-hydrodynamic (MHD) simulations. We take into account the wind from the
star, and the azimuthal and poloidal components of the magnetic field, and
investigate the PWN at different levels of magnetization (the ratio of magnetic
to matter energy-densities) in the wind. We consider the interaction of PWN
with small-scale and large-scale imhomogeneities in the ISM at different values
of magnetization. We conclude that the inhomogeneities in the ISM can change
the shapes of the bow shocks and magnetotails at different values of the
magnetization.We compare the results of our simulations with the images of the
Guitar Nebula and other PWN that show irregularities in the shapes of their bow
shocks and magnetotails. We conclude that these irregularities may be caused by
the interaction of PWN with the inhomogeneities in the ISM.
