  Pulsar wind nebulae are a possible final stage of the circumstellar evolution
of massive stars, where a fast rotating, magnetised neutron star produces a
powerful wind that interacts with the supernova ejecta. The shape of these so
called plerionic supernova remnants is influenced by the distribution of
circumstellar matter at the time of the explosion, itself impacted by the
magnetic field of the ambient medium responsible for the expansion of the
circumstellar bubble of the progenitor star. To understand the effects of
magnetization on the circumstellar medium and resulting pulsar nebulae, we
conduct 2D magnetohydrodynamical simulations. Our models explore the impact of
the interstellar medium magnetic field on the morphology of a supernova remnant
and pulsar wind nebula that develop in the circumstellar medium of massive star
progenitor in the warm phase of the Milky Ways interstellar medium. Our
simulations reveal that the jet like structures formed on both sides
perpendicularly to the equatorial plane of the pulsar, creating complex radio
synthetic synchrotron emissions. This morphology is characterized by a
rectangular like remnant, which is typical of the circumstellar medium of
massive stars in a magnetized medium, along with the appearance of a spinning
top structure within the projected rectangle. We suggest that this mechanism
may be partially responsible for the complex morphologies observed in pulsar
wind nebulae that do not conform to the typical torus, jet or bow shock, tail
shapes observed in most cases.
