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arXiv · 0710.3809

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

P. Velazquez·Y. Gomez·A. Esquivel·A. Raga
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Abstract

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 yguazu-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 \dot{M}_{csm}=5x10^{-5}M_{\odot}/yr and a terminal velocity v_{w}=10 km/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 \dot{M}_j=2.8x10^{-4} {M_{\odot}/yr (equivalent to a density of 8x10^{4} {cm}^{-3}, a velocity of 1500 km/s, a precession period of 100 yr, and a semi-aperture precession angle of 20 degrees agrees well with the observations.

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P. Velazquez, Y. Gomez, A. Esquivel, A. Raga. 2007-10-20. A precessing jet model for the PN K 3-35: simulated radio-continuum emission. https://doi.org/10.1111/j.1365-2966.2007.12510.x

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