Stationary relativistic jets

Komissarov, S. S.; Porth, Oliver; Lyutikov, Maxim

doi:10.1186/s40668-015-0013-y

Cited by 28 publications

(47 citation statements)

References 44 publications

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“…As a result, magnetised jets are more collimated and show a shorter wavelength in the oscillation of the jet boundary as compared to less magnetised jets. In addition, the increase of the magnetisation induces a higher magnetic tension and the formation of recollimation shocks is suppressed (e.g., [11,16]). …”

Section: Discussionmentioning

confidence: 99%

“…For v z ≈ c, the time-dependent 1D SRMHD solutions resemble the 2D steady-state structure of relativistic jets by substituting z = ct (see [11] for details). The 1D equations are evolved over 2000 time units.…”

Section: Srmhd Simulationsmentioning

confidence: 99%

“…The above profiles can be accompanied by any velocity and density profile. Again, we follow [11] and use for the bulk Lorentz factor:…”

Section: Srmhd Simulationsmentioning

confidence: 99%

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Radiative Signatures of Parsec-Scale Magnetised Jets

et al. 2017

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Relativistic jets are launched from the immediate vicinity of black holes and can reach kilo-parsec scales. During their evolution from the smallest to the largest scales, they encounter different physical conditions (e.g., ambient configurations and magnetic fields) which can modify their morphology and dynamics. Using state-of-the-art relativistic magneto-hydrodynamical simulations and ray-tracing algorithms, we model the dynamics of jets along with their radiation microphysics, investigating the impact of magnetisation on the jet dynamics and the observed emission. During the post-processing procedure we account for the properties of the observing array (sparse uv-plane) and the imaging algorithm, enabling a more direct comparison between simulations and groundor space-based very-long-baseline interferometry (VLBI) observations. The different jet models can be distinguished from the reconstructed radio images.

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Section: Discussionmentioning

confidence: 99%

Section: Srmhd Simulationsmentioning

confidence: 99%

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Radiative Signatures of Parsec-Scale Magnetised Jets

et al. 2017

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“…If these oscillations reflect the hydrodynamics of the flow, the pressure ratio between the jet and the external medium might be close to unity (Daly & Marscher 1988). Presence of oscillating patterns in an expanding flow is also expected for an expanding magnetized jet (Lyubarsky 2009;Komissarov et al 2015). Alternatively, these oscillations might reflect the evolution of the pinch mode or the elliptical surface mode of K-H instability (Hardee 2000;Lobanov & Zensus 2001).…”

Section: Jet Collimationmentioning

confidence: 99%

“…3). Komissarov et al (2015) have interpreted these oscillations as a standing magneto-sonic wave bouncing across the jet.…”

Section: Asymptotic Relations In the Far-zone Poynting Dominated Apprmentioning

confidence: 99%

Kinematics of the jet in M 87 on scales of 100–1000 Schwarzschild radii

Mertens

Lobanov

Walker

et al. 2016

A&A

226

266

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Context. Very long baseline interferometry (VLBI) imaging of radio emission from extragalactic jets provides a unique probe of physical mechanisms governing the launching, acceleration, and collimation of relativistic outflows. Aims. VLBI imaging of the jet in the nearby active galaxy M 87 enables morphological and kinematic studies to be done on linear scales down to ∼ 100 Schwarzschild radii (R s ). Methods. The two-dimensional structure and kinematics of the jet in M 87 (NGC 4486) have been studied by applying the Waveletbased Image Segmentation and Evaluation (WISE) method to 11 images obtained from multi-epoch Very Long Baseline Array (VLBA) observations made in January-August 2007 at 43 GHz (λ = 7 mm).Results. The WISE analysis recovers a detailed two-dimensional velocity field in the jet in M 87 at sub-parsec scales. The observed evolution of the flow velocity with distance from the jet base can be explained in the framework of MHD jet acceleration and Poynting flux conversion. A linear acceleration regime is observed up to z obs ∼ 2 mas. The acceleration is reduced at larger scales, which is consistent with saturation of Poynting flux conversion. Stacked cross correlation analysis of the images reveals a pronounced stratification of the flow. The flow consists of a slow, mildly relativistic layer (moving at β ∼ 0.5 c), associated either with instability pattern speed or an outer wind, and a fast, accelerating stream line (with β ∼ 0.92, corresponding to a bulk Lorentz factor γ ∼ 2.5). A systematic difference of the apparent speeds in the northern and southern limbs of the jet is detected, providing evidence for jet rotation. The angular velocity of the magnetic field line associated with this rotation suggests that the jet in M87 is launched in the inner part of the disk, at a distance r 0 ∼ 5 R s from the central engine.Conclusions. The combined results of the analysis imply that MHD acceleration and conversion of Poynting flux to kinetic energy play the dominant roles in collimation and acceleration of the flow in M 87.

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Substructures in Simulations of Relativistic Jet Formation

Garcia

Oliveira

2017

Braz J Phys

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Stationary relativistic jets

Cited by 28 publications

References 44 publications

Radiative Signatures of Parsec-Scale Magnetised Jets

Radiative Signatures of Parsec-Scale Magnetised Jets

Kinematics of the jet in M 87 on scales of 100–1000 Schwarzschild radii

Substructures in Simulations of Relativistic Jet Formation

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