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

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.

arXiv comment6 pages, 4 figures, accepted to MNRAS

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Cited by in corpus (13)

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• Shaping Planetary Nebulae by Light Jets
• Kinematics of the H2O masers at the centre of the PN K3-35
• Radio interferometric observations of candidate water-maser-emitting planetary nebulae
• The magnetic field toward the young planetary nebula K~3-35
• An updated catalog of OH-maser-emitting planetary nebulae
• A collimated, ionized bipolar structure and a high density torus in the young planetary nebula IRAS 17347-3139
• An asymmetric jet launching model for the protoplanetary nebula CRL 618
• H${}_2$O maser emission associated with the planetary nebula IRAS 16333$-$4807
• A Study of Radio Polarization in Protostellar Jets
• Discrete Source Survey of 6 GHz OH emission from PNe & pPNe and first 6 GHz images of K 3-35
• Shaping point- and mirror-symmetric proto-planetary nebulae by the orbital motion of the central binary system
• Dynamical modeling and the interactions with the ISM