Simulations of relativistic extragalactic jets

Duncan, G. Comer; Hughes, P. A.

doi:10.1086/187647

Cited by 134 publications

(134 citation statements)

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“…Hughes et al 2001, in preparation). Furthermore, the solver employed in the current code is a direct extension to three dimensions (with a recast from Fortran 77 to Fortran 90) of the solver described by Duncan & Hughes (1994). Evidence for the accuracy and robustness of that code comes from, in addition to its application to test problems, the general agreement between studies performed with that code and with independently constructed codes (e.g., et al 1997).…”

Section: Code V Alidation and Setupmentioning

confidence: 98%

Relativistic Jet Response to Precession and Wave‐Wave Interactions

Hardee

Hughes

Rosén

et al. 2001

ApJ

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Three-dimensional numerical simulations of the response of a Lorentz factor 2.5 relativistic jet to precession at three di †erent frequencies have been performed. Low-, moderate-, and high-precession frequencies have been chosen relative to the maximally unstable frequency predicted by a Kelvin-Helmholtz stability analysis. The transverse motion and velocity decreases as the precession frequency increases. Although the helical displacement of the jet decreases in amplitude as the precession frequency increases, a helical shock is generated in the medium external to the jet at all precession frequencies. Complex pressure and velocity structure inside the jet are shown to be produced by a combination of the helical surface and Ðrst-body modes predicted by a normal mode analysis of the relativistic hydrodynamic equations. The surface and Ðrst-body modes have di †erent wave speeds and wavelengths, are launched in phase by the periodic precession, and exhibit beat patterns in synthetic emission images. Wave (pattern) speeds range from 0.41c to 0.86c, but the beat patterns remain stationary. Thus, we Ðnd a mechanism that can produce di †erentially moving and stationary features in the jet.

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Section: Code V Alidation and Setupmentioning

confidence: 98%

Relativistic Jet Response to Precession and Wave‐Wave Interactions

Hardee

Hughes

Rosén

et al. 2001

ApJ

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“…The material is injected with a Lorentz factor γ 7.1, corresponding to a relativistic Mach number (e.g. Duncan & Hughes 1994) of M = γv/γ c s c s 17.9. The jet evolution is followed until t = 40, as shown in Fig.…”

Section: Multidimensional Testsmentioning

confidence: 99%

“…Over the last decade, high resolution shock-capturing methods of the Godunov type, successfully applied in classical fluid dynamics, have started to be employed for the case of relativistic hydrodynamics as well (Marquina et al 1992;Schneider et al 1993;Balsara 1994;Duncan & Hughes 1994;Eulderink & Mellema 1994;Font et al 1994;Dolezal & Wong 1995;Falle & Komissarov 1996;Donat et al 1998;Aloy et al 1999). These schemes are characterized by the following main features: a conservative form of the discretized equations, in order to capture weak solutions and satisfy jump relations; a reconstruction phase, to recover variables at inter-cell locations where fluxes have to be computed; an upwind phase, in which an exact or approximate solution to the local Riemann problem is found.…”

Section: Introductionmentioning

confidence: 99%

An efficient shock-capturing central-type scheme for multidimensional relativistic flows

Zanna

Bucciantini

Londrillo

2002

A&A

220

275

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Abstract. Multidimensional shock-capturing numerical schemes for special relativistic hydrodynamics (RHD) are computationally more expensive than their correspondent Euler versions, due to the nonlinear relations between conservative and primitive variables and to the consequent complexity of the Jacobian matrices (needed for the spectral decomposition in most of the approximate Riemann solvers of common use). Here an efficient and easy-to-implement three-dimensional (3-D) shockcapturing scheme for ideal RHD is presented. Based on the algorithms developed by P. Londrillo & L. Del Zanna (2000, ApJ, 530, 508) for the non-relativistic magnetohydrodynamic (MHD) case, and having in mind its relativistic MHD extension (to appear in a forthcoming paper), the scheme uses high order (third) Convex Essentially Non-Oscillatory (CENO) finite difference interpolation routines and central-type averaged Riemann solvers, which do not make use of time-consuming characteristic decomposition. The scheme is very efficient and robust, and it gives results comparable to those obtained with more sophisticated algorithms, even in ultrarelativistic multidimensional test problems.

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“…Some authors investigated the relativistic hydrodynamic jet propagation through the interstellar medium (Duncan & Hughes 1994;Martí et al 1997;Komissarov & Falle 1998;Aloy et al 1999;Rossi et al 2008). They show that the different dynamics of FR I and FR II jets may be a consequence of the jet power.…”

Section: Introductionmentioning

confidence: 99%

Relativistic spine jets from Schwarzschild black holes

Méliani¹,

Sauty²,

Tsinganos³

et al. 2010

A&A

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Context. The two types of Fanaroff-Riley (FR) radio-loud galaxies, FR I and FR II, exhibit strong jets which have different properties. These differences may be associated to the central engine and/or the external medium. Aims. The AGN classification FR I and FR II can be linked to the rate of electromagnetic Poynting flux extraction from the inner corona of the central engine by the jet. The collimation results from the distribution of the total electromagnetic energy across the jet, as compared to the corresponding distribution of the thermal and gravitational energies. Methods. We use exact solutions of the fully relativistic magnetohydrodynamical (GRMHD) equations obtained by a nonlinear separation of the variables to study outflows from a Schwarzschild black hole corona. Results. A strong correlation is found between the jet features and the energetic distribution of the plasma of the inner corona, which may be related to the efficiency of the magnetic rotator. Conclusions. It is shown that observations of FR I and FR II jets may be partially constrained by our model for spine jets. The deceleration observed in FR I jets may be associated with a low magnetic efficiency of the central magnetic rotator and an important thermal confinement by the hot surrounding medium. Conversely, the strongly collimated and accelerated FR II outflows may be self-collimated by their own magnetic field because of the high efficiency of the central magnetic rotator.

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Simulations of relativistic extragalactic jets

Cited by 134 publications

References 1 publication

Relativistic Jet Response to Precession and Wave‐Wave Interactions

Relativistic Jet Response to Precession and Wave‐Wave Interactions

An efficient shock-capturing central-type scheme for multidimensional relativistic flows

Relativistic spine jets from Schwarzschild black holes

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