Simulations of Precessing Jets

Aloy, M. A.; Martí, Juan José Ibàñez; Gómez, J. L.; Agudo, I.; Müller, Ewald; Ibáñez, Javier

doi:10.1007/978-94-017-1778-6_3

Cited by 3 publications

(3 citation statements)

References 13 publications

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“…1) and with the VLA at 22.5 GHz (Fig. 6-left) does not show the distribution expected by the models of jets advancing through the external medium, that is a perpendicular magnetic field associated with the fast spine, and a predominantly parallel magnetic field associated with the shear layer interacting with the external medium (Laing et al 1993;Aloy et al 2000). Our results could be explained if most of the polarized emission in 3C 264 comes from the shear layer of the jet, as is effectively observed at larger distances at 5 GHz (Fig.…”

Section: Transverse Structurementioning

confidence: 86%

The inner kiloparsec of the jet in 3C 264

Lara

Giovannini

Cotton

et al. 2004

A&A

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Abstract. We present new multi-frequency EVN, MERLIN and VLA observations of the radio source 3C 264, sensitive to linear scales ranging from parsec to several kiloparsecs. The observations confirm the existence of regions with different properties in the first kiloparsec of the jet. The most remarkable feature is the transition between a well collimated narrow jet at distances from the core below 80 pc, to a conical-shaped wide jet, with an opening angle of 20• . Another change of properties, consisting of an apparent deflection of the jet ridge line and a diminution of the surface brightness, occurs at a distance of ∼300 pc from the core, coincident with the radius of a ring observed at optical wavelengths. Our observations add new pieces of information on the spectrum of the radio-optical jet of 3C 264, with results consistent with a synchrotron emission mechanism and a spectrum break frequency in the infrared. Brightness profiles taken perpendicularly to the jet of 3C 264 are consistent with a spine brightened jet at distances below 100 pc from the core, and an edge-brightened jet beyond, which can be interpreted as evidence of a transverse jet velocity structure. Our observations do not allow us to distinguish between the presence of a face-on dust and gas disk at the center of the host galaxy of 3C 264, or rather an evacuated bubble. However, the properties of the jet structure, the changes in the polarization angle, and the plausible jet orientation can be naturally brought into agreement in the bubble scenario.

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Section: Transverse Structurementioning

confidence: 86%

The inner kiloparsec of the jet in 3C 264

Lara

Giovannini

Cotton

et al. 2004

A&A

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“…Simulations of these have been performed by many workers, including Aloy et al (2003), Hughes et al (2002Hughes et al ( , 1996, Hardee et al (2001Hardee et al ( , 2005Hardee et al ( , 2007, Hardee (2003), and Hardee and Rosen (2002). Included among these are Kelvin-Helmholtz instabilities, as well as waves, pinches, and bends.…”

Section: Propagation and Dynamics Of Jets At Larger Scalesmentioning

confidence: 99%

Planets, Stars and Stellar Systems

Oswalt¹,

Keel²

2013

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“…One of the first comprehensive studies regarding the effects of injection parameters on the structure of kiloparsec relativistic jets was conducted by Martí et al (1997). Several studies since have investigated various features in AGN jets such as the effects of jet composition (Scheck et al 2002) and the formation of superluminal components (Aloy et al 2003). Recent studies such as Rossi et al (2008) and Massaglia et al (2016) investigated the necessary parameters required to form FR I type jets.…”

Section: Introductionmentioning

confidence: 99%

Emission modelling of hydrodynamic AGN jet simulations

2018

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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.

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Simulations of Precessing Jets

Cited by 3 publications

References 13 publications

The inner kiloparsec of the jet in 3C 264

The inner kiloparsec of the jet in 3C 264

Planets, Stars and Stellar Systems

Emission modelling of hydrodynamic AGN jet simulations

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