2007MNRAS.382.1965V

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= 10km/s. 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 8x10⁴/cm3), a velocity of 1500km/s, a precession period of 100 yr and a semi-aperture precession angle of 20° agrees well with the observations.