Pulsar Wind nebulae are visible as bright and extended sources at a wide range of energies, with varying properties and morphology along their different evolutionary stages.
For their identification and understanding, it is extremely important to correctly describe the different stages of their evolution, where their dynamics is shaped by the interaction with different actors.
Here we will make a brief excursus through the various evolutionary phases, discussing the characteristic properties of a source in a specific phase, and what models have been used for its description.

We will conclude by discussing in particular the last evolutionary stage, that of the bow shock nebula, which is known to be connected with massive particle transfer from the source to the surrounding environment, forming either TeV halos or intriguing misaligned X-ray filaments.