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The bipolar morphology of the planetary nebula (PN) K 3 − 35 observed in radio‐continuum images was modelled with 3D hydrodynamic simulations with the adaptive grid code  yguazú‐a . We find that the observed morphology of this PN can be reproduced considering a precessing jet evolving in a dense AGB circumstellar medium, given by a mass‐loss rate  and a terminal velocity   v  w = 10 km s −1  . Synthetic thermal radio‐continuum maps were generated from numerical results for several frequencies. Comparing the maps and the total fluxes obtained from the simulations with the observational results, we find that a model of precessing dense jets, where each jet injects material into the surrounding CSM at a rate  (equivalent to a density of 8 × 10 4  cm −3 ), a velocity of 1500 km s −1 , a precession period of 100 yr and a semi‐aperture precession angle of 20° agrees well with the observations.

A precessing jet model for the PN K 3 − 35: simulated radio‐continuum emission