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

TL;DR

This paper models the bipolar morphology of planetary nebula K 3-35 using 3D hydrodynamic simulations of a precessing jet, successfully reproducing observed radio-continuum features and fluxes.

Contribution

It introduces a detailed 3D hydrodynamic model of a precessing jet to explain the morphology and radio emission of PN K 3-35, aligning simulations with observations.

Findings

Precessing dense jets reproduce observed nebula morphology.

Simulated radio maps match observational fluxes across frequencies.

Jet parameters like precession period and angle are constrained by the model.

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.