Three-Dimensional Simulations of Bi-Directed Magnetohydrodynamic Jets Interacting With Cluster Environments

O’Neill, Sean M.; Jones, T. W.

doi:10.1088/0004-637x/710/1/180

Cited by 58 publications

(59 citation statements)

References 82 publications

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“…When the jets penetrate to too large distances no fat bubbles are formed, while in intermediate cases elongated bubbles and/or bubbles detached from the center are formed (e.g., Basson & Alexander 2003;Omma et al 2004;Heinz et al 2006;Vernaleo & Reynolds 2006;Alouani Bibi et al 2007;O'Neill & Jones 2010;Mendygral et al 2011Mendygral et al , 2012.…”

Section: The Jetsmentioning

confidence: 99%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

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I review the influence jets and the bubbles they inflate might have on their ambient gas as they operate through a negative jet feedback mechanism (JFM). I discuss astrophysical systems where jets are observed to influence the ambient gas, in many cases by inflating large, hot, and low-density bubbles, and systems where the operation of the JFM is still a theoretical suggestion. The first group includes cooling flows in galaxies and clusters of galaxies, star-forming galaxies, young stellar objects, and bipolar planetary nebulae. The second group includes core collapse supernovae, the common envelope evolution, the grazing envelope evolution, and intermediate luminosity optical transients. The suggestion that the JFM operates in these four types of systems is based on the assumption that jets are much more common than what is inferred from objects where they are directly observed. Common to all eight types of systems reviewed here is the presence of a compact object inside an extended ambient gas. The ambient gas serves as a potential reservoir of mass to be accreted on to the compact object. If the compact object launches jets as it accretes mass, the jets might reduce the accretion rate as they deposit energy to the ambient gas, or even remove the entire ambient gas, hence closing a negative feedback cycle.

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Section: The Jetsmentioning

confidence: 99%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

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“…(e.g. Brüggen & Kaiser 2002; De Young 2003; Brighenti & Mathews 2003; Ruszkowski et al 2007; Sijacki et al 2008; Xu et al 2009; O’Neill & Jones 2010; Scannapieco & Brüggen 2010).…”

Section: Physical Effects On the Entropy Productionmentioning

confidence: 99%

The entropy core in galaxy clusters: numerical and physical effects in cosmological grid simulations

Vazza¹

2010

Monthly Notices of the Royal Astronomical Society

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A flat distribution of low gas entropy in the core region of galaxy clusters is a feature commonly found in Eulerian cosmological simulations, at variance with most standard simulations of smoothed particle hydrodynamics fashion. From the literature, it is still unclear whether this difference is entirely due to numerical artefacts (e.g. spurious transfer from gravitational energy to thermal energy), physical mechanisms (e.g. enhanced mixing in Eulerian codes) or a mixture of both. This issue is related to many still open lines of research in the characterization of the dynamical evolution of the baryons in galaxy clusters: the origin of the cool‐core/non‐cool‐core bi‐modality, the diffusion of metals within galaxy clusters, the interplay between active galactic nuclei (AGN) and the intra‐cluster medium, etc. In this work, we aim at constraining to what extent the entropy core is affected by numerical effects, and which are the physical reasons for its production in cosmological runs. To this end, we run a set of 30 high‐resolution re‐simulations of a ∼3 × 1014 M⊙ h−1 cluster of galaxies with a quiet dynamical history, using modified versions of the cosmological adaptive mesh refinement code enzo and investigating many possible (physical and numerical) details involved in the production of entropy in simulated galaxy clusters. We report that the occurrence of a flat entropy core in the innermost region of a massive cluster is mainly due to hydrodynamical processes resolved by the numerical code (e.g. shocks and mixing motions) and that additional spurious effects of numerical origin (e.g. artificial heating due to softening effects) affect the size and level of the entropy core only in a minor way. Using Lagrangian tracers we show that the entropy profile of non‐radiative simulations is produced by a mechanism of ‘sorting in entropy’ which takes place with regularity during the cluster evolution. The evolution of tracers illustrates that the flat entropy core is caused by physical mixing of subsonic motions (mostly driven by accreted sub‐clumps) within the shallow inner cluster potential. Several re‐simulations were also produced for the same cluster object with the addition of radiative cooling, uniform pre‐heating at high redshift (z= 10) and late (z < 1) thermal energy feedback from AGN activity in the cluster, in order to assess the effects of such mechanisms on the final entropy profile of the cluster. We report on the infeasibility of balancing the catastrophic cooling (and recovering a flat entropy profile) by means of the investigated trials for AGN activity alone, while for a sub‐set of pre‐heating models, or AGN feedback plus pre‐heating models, a flat entropy distribution similar to non‐radiative runs can be obtained with a viable energy requirement. Complementary analysis is presented also for a major merger cluster, obtaining similar results and achieving a generally good consistency with X‐ray data for the entropy distribution in real galaxy clusters.

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“…Images as in Figure 1 have inspired many theoretical studies of Fanaroff-Riley II (FRII) jets and their cocoons (e.g., Blandford & Rees 1974;Scheuer 1974;Kaiser & Alexander 1997;Clarke et al 1997;Carvalho & O'Dea 2002;Carvalho et al 2005;Krause, 2005;Saxton et al 2002;O'Neill & Jones 2010;Huarte-Espinosa et al 2011). Here we describe approximate calculations emphasizing the dynamical evolution of material inside the radio lobes.…”

Section: Introductionmentioning

confidence: 99%

Dynamics Inside the Radio and X-Ray Cluster Cavities of Cygnus a and Similar Frii Sources

Mathews

Guo

2012

ApJ

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We describe approximate axisymmetric computations of the dynamical evolution of material inside radio lobes and X-ray cluster gas cavities in Fanaroff-Riley II (FRII) sources such as Cygnus A. All energy is delivered by a jet to the lobe/cavity via a moving hotspot where jet energy dissipates in a reverse shock. Our calculations describe the evolution of hot plasma, cosmic rays (CRs), and toroidal magnetic fields flowing from the hotspot into the cavity. Many important observational features are explained. Gas, CRs, and field flow back along the cavity surface in a "boundary backflow" consistent with detailed FRII observations. Computed ages of backflowing CRs are consistent with observed radio-synchrotron age variations only if shear instabilities in the boundary backflow are damped and we assume this is done with viscosity of unknown origin. We compute a faint thermal jet along the symmetry axis and suggest that it is responsible for redirecting the Cygnus A nonthermal jet. Magnetic fields estimated from synchrotron self-Compton (SSC) X-radiation observed near the hotspot evolve into radio lobe fields. Computed profiles of radio-synchrotron lobe emission perpendicular to the jet reveal dramatically limb-brightened emission in excellent agreement with FRII observation, although computed lobe fields exceed those observed. Strong winds flowing from hotspots naturally create kiloparsec-sized spatial offsets between hotspot nonthermal X-ray inverse Compton (IC-CMB) emission and radio-synchrotron emission that peaks 1-2 kpc ahead where the field increases due to wind compression. In our computed version of Cygnus A, nonthermal X-ray emission increases from the hotspot (some IC-CMB, mostly SSC) toward the offset radio-synchrotron peak (mostly SSC).

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Three-Dimensional Simulations of Bi-Directed Magnetohydrodynamic Jets Interacting With Cluster Environments

Cited by 58 publications

References 82 publications

The jet feedback mechanism (JFM) in stars, galaxies and clusters

The jet feedback mechanism (JFM) in stars, galaxies and clusters

The entropy core in galaxy clusters: numerical and physical effects in cosmological grid simulations

Dynamics Inside the Radio and X-Ray Cluster Cavities of Cygnus a and Similar Frii Sources

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