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The dynamics, energetics and evolution of pulsar wind nebulae (PWNe) andsupernova remnants (SNRs), are strongly affected by their magnetic fieldstrength and distribution. They are usually strong, extended, sources ofnon-thermal X-ray radiation, producing intrinsically polarised radiation. Theenergetic wind around pulsars produces a highly-magnetised, structured flow,often displaying a jet and a torus and different features (i.e. wisps, knots).This magnetic-dominant wind evolves as it moves away from the pulsarmagnetosphere to the surrounding large-scale nebula, becoming kinetic-dominant.Basic aspects such how this conversion is produced, or how the jets and torusare formed, as well as the level of turbulence in the nebula are still unknown.Likewise, the processes ruling the acceleration of particles in shell-like SNRsup to 1e15 eV, including the amplification of the magnetic field, are not clearyet. Imaging polarimetry in this regard is crucial to localise the regions ofshock acceleration and to measure the strength and the orientation of themagnetic field at these emission sites. X-ray polarimetry with the X-rayImaging Polarimetry Explorer (XIPE) will allow the understanding of themagnetic field structure and intensity on different regions in SNRs and PWNe,helping to unveil long-standing questions such as i.e. acceleration of cosmicrays in SNRs or magnetic-to-kinetic energy transfer. SNRs and PWNe alsorepresent the largest population of Galactic very-high energy gamma-raysources, therefore the study of their magnetic distribution with XIPE willprovide fundamental ingredients on the investigation of those sources at veryhigh energies. We will discuss the physics case related to SNRs and PWNe andthe expectations of the XIPE observations of some of the most prominent SNRsand PWNe.

Unveiling the Magnetic Structure of VHE SNRs/PWNe with XIPE, the X-ray Imaging-Polarimetry Satellite