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Emission modelling of hydrodynamic AGN jet simulations

Published online by Cambridge University Press:  07 April 2020

Izak P. van der Westhuizen ,
Brian van Soelen  and
Petrus J. Meintjes
Izak P. van der Westhuizen
Affiliation:
Department of Physics, University of the Free State, PO Box 339, Bloemfontein9300, South Africa, email: vanderwesthuizenip@ufs.ac.za
Brian van Soelen
Affiliation:
Department of Physics, University of the Free State, PO Box 339, Bloemfontein9300, South Africa, email: vanderwesthuizenip@ufs.ac.za
Petrus J. Meintjes
Affiliation:
Department of Physics, University of the Free State, PO Box 339, Bloemfontein9300, South Africa, email: vanderwesthuizenip@ufs.ac.za
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Abstract

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Radio-loud Active Galactic Nuclei (AGN) produce relativistic jets that can be modelled with relativistic hydrodynamic (RHD) simulations. In this study we present two such simulations of jets, used to investigate the parameters required to reproduce structures consistent with both FR I and FRII jets. In the first simulation a Lorentz factor of 10 and supersonic flow of Mach 30 were chosen, while for the second simulation a Lorentz factor of 1.0014 with a supersonic flow of Mach 4 was used. Over similar distances scales the first case shows a well collimated beam with a strong shock at the interface between the jet and ambient medium while the second case shows a less stable beam and a larger cocoon. To determine whether the simulated physical structures are consistent with the observed FR I/II jets, the synchrotron emission has been calculated to produce radio maps at a single frequency of 1.5 GHz.

Keywords

HydrodynamicActive Galactic NucleiRelativistic jets
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S342: Perseus in Sicily: From Black Hole to Cluster Outskirts , May 2018 , pp. 209 - 213
Copyright
© International Astronomical Union 2020

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