At the end of their lives, low and intermediate-mass stars scatter their envelope throughout the interstellar medium via a stellar wind.
Recent high-spatial resolution observations reveal that the winds of these evolved AGB stars typically possess a high degree of complexity, including spirals, disks, clumps, etc.
With 3D hydrodynamical PHANTOM models, we show how these wind structures can be formed when one or multiple stellar or planetary companions are gravitationally interacting with the AGB outflow.
Our simulations hence offer us a novel gateway to unravel how and by which binary/triple configurations of the intricate wind structures in the actual ALMA observations can be created.

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