A Comparison of the Morphology and Stability of Relativistic and Nonrelativistic Jets

Rosén, Å.; Hughes, P. A.; Duncan, G. Comer; Hardee, Philip E.

doi:10.1086/307143

Cited by 73 publications

(95 citation statements)

References 26 publications

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“…Fig. 18 shows a comparison between our models and the simple analytical model presented by Rosen et al (1999). This model predicts a value for the ratio of lobe radius (R l ) to jet radius (R j ) based upon the jet's values of γ and η r .…”

Section: Discussionmentioning

confidence: 97%

Numerical modelling of the lobes of radio galaxies in cluster environments – III. Powerful relativistic and non-relativistic jets

English

Hardcastle

Krause

2016

Mon. Not. R. Astron. Soc.

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We present results from two suites of simulations of powerful radio galaxies in poor cluster environments, with a focus on the formation and evolution of the radio lobes. One suite of models uses relativistic hydrodynamics and the other relativistic magnetohydrodynamics; both are set up to cover a range of jet powers and velocities. The dynamics of the lobes are shown to be in good agreement with analytical models and with previous numerical models, confirming in the relativistic regime that the observed widths of radio lobes may be explained if they are driven by very light jets. The ratio of energy stored in the radio lobes to that put into the intracluster gas is seen to be the same regardless of jet power, jet velocity or simulation type, suggesting that we have a robust understanding of the work done on the ambient gas by this type of radio source. For the most powerful jets we at times find magnetic field amplification by up to a factor of two in energy, but mostly the magnetic energy in the lobes is consistent with the magnetic energy injected. We confirm our earlier result that for jets with a toroidally injected magnetic field, the field in the lobes is predominantly aligned with the jet axis once the lobes are well developed, and that this leads to radio flux anisotropies of up to a factor of about two for mature sources. We reproduce the relationship between 151-MHz luminosity and jet power determined analytically in the literature.

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Section: Discussionmentioning

confidence: 97%

Numerical modelling of the lobes of radio galaxies in cluster environments – III. Powerful relativistic and non-relativistic jets

English

Hardcastle

Krause

2016

Mon. Not. R. Astron. Soc.

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“…(For an introduction to the literature on this work one may consult the recent papers of Agudo et al (2001), Rosen, Hughes, & Duncan (1999), and Komissarov & Falle (1997).) The answer is yes for several reasons:…”

Section: Relationship To Numerical Simulations Of Relativistic Jetsmentioning

confidence: 99%

The Evolution of Shocks in Blazar Jets

Bicknell

Wagner²

2002

Publ. – Astron. Soc. Aust

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We consider the shock structures that can arise in blazar jets as a consequence of variations in the jet flow velocity. There are two possible cases: (1) A double shock system consisting of both a forward and reverse shock (2) A single shock (either forward or reverse) together with a rarefaction wave. These possibilities depend upon the relative velocity of the two different sections of jet. Using previously calculated spherical models for estimates of the magnetic field and electron number density of the emission region in the TeV blazar Markarian 501, we show that this region is in the form of a thin disk, in the plasma rest frame. It is possible to reconcile spectral and pair opacity constraints for MKN 501 for Doppler factors in the range of 10--20. This is easiest if the corrections for TeV absorption by the infrared background are not as large as implied by recent models.Comment: 19 pages, 8 figures, accepted for publication in PASA, 19, No.1, AGN Variability across the Electromagnetic Spectru

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“…Low jet densities are needed to get large radio cocoon and bow shock widths. Based on the results from a grid of simulations and comparison to the radio and X-ray data of the radio galaxy Cygnus A (Carilli & Barthel 1996;Smith et al 2002), a density contrast of roughly η < 10 −3 has been claimed for this source (Rosen et al 1999;Krause 2003). All these simulations have been carried out in axisymmetry and a scale of a few dozen jet radii.…”

Section: Introductionmentioning

confidence: 99%

Very light jets II: Bipolar large scale simulations in King atmospheres

Krause¹

2005

A&A

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Abstract. Hydrodynamic jets, underdense with respect to their environment by a factor of up to 10 4 , were computed in axisymmetry as well as in 3D. They finally reached a size of up to 220 jet radii, corresponding to a 100 kpc sized radio galaxy. The simulations are "bipolar", involving both jets. These are injected into a King type density profile with small stochastic density variations. The back-reaction of the cocoons on the beams in the center produces armlength asymmetries of a few percent, with the longer jets on the side with the higher average density. Two distinguishable bow shock phases were observed: an inner elliptical part, and a later cylindrical, cigar-like phase, which is known from previous simulations. The sideways motion of the inner elliptical bow shock part is shown to follow the law of motion for spherical blast waves also in the late phase, where the aspect ratio is high, with good accuracy. X-ray emission maps are calculated and the two bow shock phases are shown to appear as rings and elongated or elliptical regions, depending on the viewing angle. Such structures are observed in the X-ray data of several radio galaxies (e.g. in Abell 2052 and Hercules A), the best example being Cygnus A. In this case, an elliptical bow shock is infered from the observations, a jet power of 10 47 erg/s is derived, and the Lorentz factor can be limited to Γ > 10. Based on the simulation results and the comparison to the observations, the emission line gas producing the alignment effect in radio galaxies at high redshift is suggested to be cooled gas entrained over the cocoon boundary.

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A Comparison of the Morphology and Stability of Relativistic and Nonrelativistic Jets

Cited by 73 publications

References 26 publications

Numerical modelling of the lobes of radio galaxies in cluster environments – III. Powerful relativistic and non-relativistic jets

Numerical modelling of the lobes of radio galaxies in cluster environments – III. Powerful relativistic and non-relativistic jets

The Evolution of Shocks in Blazar Jets

Very light jets II: Bipolar large scale simulations in King atmospheres

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