The inner regions of galaxies are rich in gas and stars that can interact with the jet and produce high-energy non-thermal emission, as well as significantly mass-load the jet. We focus on a population of stars with strong winds, which accumulate material around the star outside the jet, confined by pressure equilibrium with the environment, in the form of a bubble. When these bubbles reach the jet, a shock is produced in the external bubble layer, which may cause part of the material to be peeled away and carried upstream at the contact discontinuity. Part of the remaining bubble may penetrate the jet, and eventually detach and accelerate up to relativistic speeds, producing non-thermal emission.