a) Sketch of the pulsar high-mass binary scenario on scales larger than the binary system. The star (S) and pulsar (P) shocked winds trace a spiral-shape due to the Coriolis force and the pulsar orbital motion. Eventually, both shocked winds mix due to Kelvin-Helmholtz instabilities, and the spiral arms merge. b) Cartoon of the bubble (case η < 1) driven by the shocked flows formed within the binary system (BS) and made of pulsar- and stellar-wind material. The bubble expands and accelerates, eventually terminating in a shock where its ram pressure is equal to the pressure of the SNR or the shocked ISM for old enough sources. This occurs at the contact discontinuity (CD).