Instabilities of relativistic jets

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1 Instabilities of relativistic jets G. Bodo INAF Osservatorio Astrofisico di Torino, Italy A. Mignone, P. Rossi, G. Mamatsashvili, S. Massaglia, A. Ferrari

2 show f Universality of relativistic jet phenomenon High energy sources AGN Microquasars GRB Pulsar wind nebulae Universality of relativistic jet phenomenon Microquasar is a scaled down (by a factor of 10 6 ) version NW jet of active galactic nuclei M Microquasars Universality of relativistic jet phenomenon 1. Radio galaxies and quasars M 87 Anvil) s and nd SE jet Superluminal motion in microquasar GRS ; V apparent =1.5c ong the jets; Similar physical processes may operate in all these objects ith v/c 0.4 slowing

3 HOW JETS ARE ACCELERATED? Compact object + accretion disc Current models for the jet acceleration are related to the interplay of magnetic field and rotation. The flow starts as Poynting dominated->matter dominated at large distances Twisted magnetic field Velocity shear Rotating jets Blandford&Payne 1982 Instabilities

4 WHAT INSTABILITIES DO? Instabilities dissipation radiation Instabilities morphologies Instabilities momentum transfer, jet deceleration formation of velocity structures Instabilities jet disruption

5 Jet Wobbling High resolution VLBI observations of some AGN jets show regular or irregular swings of innermost jet structural position angle (jet wobbling). SE jet morphology is S shaped and show remarkable time variability: Morphological features in jets: knots, wiggling Parsec scale AGN jet curvatures and helical-like structures (inner parsec or large scale) are believed to be triggered by changes in direction at the jet nozzle. Physical origin of jet wobbling (Agudo 2009) Accretion disk precession Orbital motion of accretion system (binary BH?) Jet instabilities evidence for some kind of flow instability (Current Driven?) Crab Nebula Ultra fast TeV variability in Blazars Emitter compact and very large Lorentz factors Very compact dissipation region ast TeV Flare in Blazars es are observed in s sort as 3M 9 hour on to escape pair quired (Begelman,, Mrk 501 show minal ejections mpact and WHAT OBSERVATIONS TELL US? PKS (Aharonian et al. 2007) See also Mrk501, PKS P.A. 15 GHz VLBI image of 4C Position angle oscillation of 3C273 Velocity structure in jets year Fast spine surrounded by a slower layer

6 HOW DO WE STUDY INSTABILITIES? Linear analysis What are the dominant modes of instabilities? What are the driving forces? Only valid when perturbations are small NUMERICAL SIMULATIONS Numerical Modeling LOCAL MODELS (small section of the jet) elativistic simulations: lobal models (full jet propagation) ckinney & Blandford (2009), ignone et al. (2010) GLOBAL MODELS (full jet propagation)

7 LINEAR ANALYSIS EQUILIBRIUM Cold case No pressure We consider a case where the current is concentrated inside the jet return current very far from the jet PARAMETERS magnetization Pitch

8 Bodo et al LINEAR ANALYSIS RESULTS Kelvin Helmholtz Velocity shear Current driven Twisted field k P(r) = 1 B Kink modes m=1

9 WHAT ABOUT ROTATION? STABILIZATION OF CURRENT DRIVEN MODE, BUT NEW MODES Kelvin Helmholtz Rotation

10 LOCAL ANALYSIS (non relativistic, magnetically dominated jets) We take a local section of the jet, periodic boundary conditions along the jet INITIAL EQUILIBRIUM (no rotation)

11 EVOLUTION

12 ENERGY EVOLUTION

13 GLOBAL ANALYSIS JET PROPAGATION Jet Injection + perturbations z x outflow outflow outflow First case with no magnetic field: jet deceleration and formation of a spine layer structure Turbulent structure driven by Kelvin-Helmholtz instabilities y M=3 h=10 2 M=3 h=10 4 M=30 h=10 2

14 Mixing by shear instabilities A = 10, M = 3, h = 10 2 B = 10, M = 3, h = 10 4 Relativistic spine surrounded by a turbulent mixing layer E = 10, M = 30, h = 10 2

15 Comparison with observations Emissivity integration along the line of sight at different projection angles Doppler boosting = 20º = 60º

16 Poloidal Magnetized Models: Tracer distribution RHD (Hydro) Toroidal 2Dl Toroidal 3D

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20 THANK YOU