Numerical simulations of magnetized jets

Lind, K. R.; Payne, D. G.; Meier, David L.; Blandford, R. D.

doi:10.1086/167779

Cited by 139 publications

(149 citation statements)

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“…We note that while the jet cylinder radius in these simulations generally increases with time (due to the central densities falling), we also expect the jet to broaden naturally as it propagates to larger distances, a result which has also been found by previous work (e.g. Norman et al 1982;Lind et al 1989;Krause & Camenzind 2001;Krause 2003) and is the likely reason why the evolution of jet length found in our simulations differs somewhat from that predicted by simple analytical arguments (e.g. Begelman & Cioffi 1989).…”

Section: Jet Propagation: Comparison To Analytical Modelssupporting

confidence: 87%

AGN jet feedback on a moving mesh: cocoon inflation, gas flows and turbulence

Bourne¹,

Sijacki

2017

Monthly Notices of the Royal Astronomical Society

105

101

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In many observed galaxy clusters, jets launched by the accretion process on to supermassive black holes, inflate large-scale cavities filled with energetic, relativistic plasma. This process is thought to be responsible for regulating cooling losses, thus moderating the inflow of gas on to the central galaxy, quenching further star formation and maintaining the galaxy in a red and dead state. In this paper, we implement a new jet feedback scheme into the moving mesh-code arepo, contrast different jet injection techniques and demonstrate the validity of our implementation by comparing against simple analytical models. We find that jets can significantly affect the intracluster medium (ICM), offset the overcooling through a number of heating mechanisms, as well as drive turbulence, albeit within the jet lobes only. Jet-driven turbulence is, however, a largely ineffective heating source and is unlikely to dominate the ICM heating budget even if the jet lobes efficiently fill the cooling region, as it contains at most only a few percent of the total injected energy. We instead show that the ICM gas motions, generated by orbiting substructures, while inefficient at heating the ICM, drive large-scale turbulence and when combined with jet feedback, result in line-ofsight velocities and velocity dispersions consistent with the Hitomi observations of the Perseus cluster.

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Section: Jet Propagation: Comparison To Analytical Modelssupporting

confidence: 87%

AGN jet feedback on a moving mesh: cocoon inflation, gas flows and turbulence

Bourne¹,

Sijacki

2017

Monthly Notices of the Royal Astronomical Society

105

101

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“…In his initial models for compact symmetric objects, Begelman (1996) conjectured that the evolution of a lobe would occur in such a way that the mean hot-spot pressure would be approximately a constant factor (here denoted by ζ ) times the cocoon pressure. He justified this by examining the initial stages of simulations by Lind et al (1989) concluding that ζ ≈ 2; the conjecture has since been verified in detail for the propagation of overpressured lobes (Carvalho & O'Dea 2002a, 2002b; see also O'Dea these proceedings). Bicknell, Dopita, & O'Dea (1997, hereafter BDO) refined the Begelman (1996) model by allowing for expansion losses.…”

Section: Evolution Of Gps and Css Sourcesmentioning

confidence: 93%

GPS and CSS Sources — Theory and Modelling

Bicknell

Saxton

Sutherland³

2003

Publ. – Astron. Soc. Aust

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Abstract:We review theoretical ideas that seem to be currently important for the physics of GPS and CSS radio sources. These include models for their evolution, the production of emission lines, and the origin of the low frequency turnover. We also describe the initial phases of a program of simulations that is aimed at understanding the radiative interactions between jets, lobes, and dense clouds in the nuclei of these objects.

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“…In the past, environments have been taken to have a constant density profile (Norman et al 1982;Kössl & Müller 1988;Lind et al 1989), which may be acceptable for the early growth of the lobes but is clearly not over the length scales the radio lobes are observed to reach. This was later improved upon by considering more realistic beta model environments (Reynolds, Heinz & Begelman 2002;Basson & Alexander 2003;Krause 2005) or an environment derived from a simulation of a dynamically active cluster (Heinz et al 2006).…”

Section: Introductionmentioning

confidence: 99%

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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Numerical simulations of magnetized jets

Cited by 139 publications

References 0 publications

AGN jet feedback on a moving mesh: cocoon inflation, gas flows and turbulence

AGN jet feedback on a moving mesh: cocoon inflation, gas flows and turbulence

GPS and CSS Sources — Theory and Modelling

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

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