Schematic pictures of the three physical configurations modeled in this work. Panel (a): Scenario A consists of an inner blob, originating from either the (outflowing) corona or an internal shock, and a jet blob, produced by either an internal or termination shock. Both blobs lie along the same direction but are located at different heights and move with distinct velocities. Panel (b): Scenario B features a primary jet emission region surrounded by the dense stellar-wind environment of the companion star. In the static external emission zone, charged particles escaping from the jet interact with the stellar wind. Panel (c): Scenario C considers the contribution from the extended jet. Within the large-scale, static external shell, particles that have escaped from the jet blob interact with the surrounding parsec-scale environment.