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Stability of Magnetized Relativistic Jets

Stability of Magnetized Relativistic Jets. Yosuke Mizuno Center for Space Plasma and Aeronomic Research (CSPAR) University of Alabama in Huntsville Collaborators P. E. Hardee (UA), Y. Lyubarsky (Ben-Gurion Univ), K.-I. Nishikawa (NSSTC/UAH). Mizuno, Hardee, & Nishikawa. 2007, ApJ, 662,835

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Stability of Magnetized Relativistic Jets

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  1. Stability of Magnetized Relativistic Jets Yosuke Mizuno Center for Space Plasma and Aeronomic Research (CSPAR) University of Alabama in Huntsville Collaborators P. E. Hardee (UA), Y. Lyubarsky (Ben-Gurion Univ), K.-I. Nishikawa (NSSTC/UAH) Mizuno, Hardee, & Nishikawa. 2007, ApJ, 662,835 Mizuno, Lyubarsky, Nishikawa, & Hardee. 2009, ApJ, 700, 684 Mizuno, Hardee, & Nishikawa, 2010, ApJ, submitted

  2. Relativistic Jets Radio observation of M87 jet • Relativistic jets: outflow of highly collimated plasma • Microquasars, Active Galactic Nuclei, Gamma-Ray Bursts, Jet velocity ～c • Generic systems: Compact object（White Dwarf, Neutron Star, Black Hole）+ Accretion Disk • Key Issues of Relativistic Jets • Acceleration & Collimation • Propagation & Stability • Modeling for Jet Production • Magnetohydrodynamics (MHD) • Relativity (SR or GR) • Modeling of Jet Emission • Particle Acceleration • Radiation mechanism

  3. 15 GHz VLBI image of 4C+12.50 Jet Wobbling • High resolution VLBI observations of some AGN jets show regular or irregular swings of innermost jet structural position angle (jet wobbling). • 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 Position angle oscillation of 3C273 P.A. year

  4. Instability of Relativistic Jets • When jets propagate outward, there are possibility to grow of two major instabilities • Kelvin-Helmholtz (KH) instability • Important at the shearing boundary flowing jet and external medium • Current-Driven (CD) instability • Important in twisted magnetic field • Interaction of jets with external medium caused by such instabilities leads to the formation of shocks, turbulence, acceleration of charged particles etc. • Used to interpret many jet phenomena • quasi-periodic wiggles and knots, filaments, limb brightening, jet disruption etc Limb brightening of M87 jets (observation)

  5. Key Questions of Jet Stability • When jets propagate outward, there are possibility to grow of two instabilities • Kelvin-Helmholtz (KH) instability • Current-Driven (CD) instability • How do jets remain sufficiently stable? • What are the Effects & Structure of KH / CD Instability in particular jet configuration (such as spine-sheath configuration)? • We investigate these topics by using 3D relativistic MHD simulations

  6. 1. Kelvin-Helmholtz Instability of Magnetized Spine-Sheath Relativistic Jets

  7. Spine-Sheath Relativistic Jets (observations) M87 Jet: Spine-Sheath (two-component) Configuration? HST Optical Image (Biretta, Sparks, & Macchetto 1999) VLA Radio Image (Biretta, Zhou, & Owen 1995) Typical Proper Motions > c Optical ~ inside radio emission Jet Spine ? Typical Proper Motions < c Radio ~ outside optical emission Sheath wind ? • Observations of QSOs show the evidence of high speed wind （~0.1-0.4c）(Pounds et al. 2003): • Related to Sheath wind • Spine-sheath configuration proposed to explain • TeV Blazars (Ghisellini et al. 2005, Ghisellini & Tavecchio 2008) • TeV emission in M87 (Taveccio & Ghisellini 2008) • limb brightening in M87, Mrk501jets （Perlman et al. 2001; Giroletti et al. 2004） • broadband emission in PKS 1127-145 jet (Siemiginowska et al. 2007)

  8. Spine-Sheath Relativistic Jets (GRMHD Simulations) • In many GRMHD simulation of jet formation (e.g., Hawley & Krolik 2006, McKinney 2006, Hardee et al. 2007), suggest that • a jet spine driven by the magnetic fields threading the ergosphere • may be surrounded by a broad sheath wind driven by the magnetic fields anchored in the accretion disk. Non-rotating BH Fast-rotating BH Spine Sheath Total velocity Disk Disk Jet/Wind BH Jet Disk Jet/Wind Density distribution (McKinney 2006) (Hardee, Mizuno & Nishikawa 2007)

  9. Stabilities of magnetized spine-sheath jets against KH modes • From previous works, KH instability is stable in sub-Alfvenic jet regime (magnetic field is strong). • But observed jet is kinetic energy is dominated (magnetic energy is week) and jet is super-Alfvenic. • Is relativistic jet unstable for KH mode everywhere? • New idea: spine-sheath configuration • Relativistic MHD jet cases are not fully addressed in both linear analysis and MHD simulation -> present work

  10. Initial Condition Mizuno, Hardee & Nishikawa, 2007 • Cylindrical super-Alfvenic jet established across the computational domain with a parallel magnetic field (stable against CD instabilities) • Solving 3D RMHD equations in Cartesian coordinates • (using Minkowski spacetime) • Jet (spine): ujet = 0.916 c (γj=2.5), jet = 2 ext (dense, cold jet) • External medium (sheath):uext = 0 (static), 0.5c (sheath wind) • Jet spine precessed to break the symmetry (frequency, w=0.93) • RHD: weakly magnetized (sound velocity > Alfven velocity) • RMHD: strongly magnetized (sound velocity < Alfven velocity) • Numerical box and computational zones • -3 rj< x,y< 3rj, 0 rj< z < 60 rj (Cartesian coordinates) with 60*60*600 zones, (1rj=10 zones)

  11. Global Structure 3D isovolume density at t=60 External wind (spine-sheath) case No wind case vj • The precession perturbation from jet inlet leads to grow of KH instability and it disrupts jet structure in non-linear phase. • Growth/damp of KH instability and jet structure is different in each cases.

  12. Effect of magnetic field and sheath wind 1D radial velocity profile along jet ue=0.0 ue=0.5c ue=0.0 ue=0.5c • The sheath flow reduces the growth rate of KH modes and slightly increases the wave speed and wavelength as predicted from linear stability analysis. • The magnetized sheath reduces growth rate relative to the weakly magnetized case • The magnetized sheath flow damped growth of KH modes. • Criterion for damped KH modes: • (linear stability analysis)

  13. 2. Current Driven kink instability of static plasma column

  14. CD Kink Instability • In configurations with strong toroidal magnetic fields, current-driven (CD) kink mode (m=1) is unstable. • This instability excites large-scale helical motions that can be strongly distort or even disrupt the system • For static cylindrical force-free equilibria, well known Kurskal-Shafranov (KS) criterion • Unstable wavelengths: l > |Bp/Bf |2pR • However, rotation and shear motion could significant affect the instability criterion Schematic picture of CD kink instability 3D MHD simulation for propagating jet (Nakamura & Meier. 2004)

  15. Previous work for CD kink instability • For relativistic force-free configuration • Linear mode analysis provides conditions for the instability but say little about the impact instability has on the system(Istomin & Pariev (1994, 1996), Begelman(1998), Lyubarskii(1999), Tomimatsu et al.(2001), Narayan et al. (2009)) • Instability of potentially disruptive kink mode must be followed into the non-linear regime • Helical structures have been found in Newtonian /relativistic simulations of magnetized jets formation and propagation (e.g., Nakamura & Meier 2004; Moll et al. 2008; McKinney & Blandford 2009; Mignone et al. 2010)

  16. Purpose • We investigate detail of non-linear behavior of relativistic CD kink instability • Relativistic: not only moving systems with relativistic speed but any with magnetic energy density comparable to or greater than the plasma energy density. • We start from static configurations because in the case of interest, the free energy is the magnetic energy, not kinetic energy • Static configuration (in generally, rigidly moving flows considered in the proper frame) are the simplest ones for studying the basic properties of the kink instability.

  17. Initial Condition Mizuno et al. 2009 • Static force-free equilibrium helical magnetic field (unstable against CD kink instability) • Magnetic pitch (P=RBz/Bf): constant, increase, decrease • Density profile: constant or decrease (r=r0 B2) • Numerical box:-2L < x, y < 2L, 0 < z < 2L(Cartesian coordinates:160 x 160 x 80 zones) • Boundary: periodic in axial (z) direction • Small velocity perturbation with m=1(-1) andn=1(-1) modes

  18. Initial Force-Free Configuration Radial profile Magnetic pitch Black: constant density Red: decreasing density Solid: constant pitch dotted: increase pitch Dashed: decrease pitch Sound velocity Alfven velocity density

  19. 3D Structure (Decrease density with Constant pitch) • Displacement of the initial force-free helical magnetic field leads to a helically twisted magnetic filament around the density isosurface by CD kink instability • Slowly continuing outwards radial motion is confined to a lower density sheath around the high density core Color: density White line: magnetic field lines

  20. Dependence on pitch profile tA: Alfven crossing time Constant pitch Decrease pitch Increase pitch • Constant pitch: Amplitude growth slows at later time. • Increase pitch: 3D density structure looks similar to constant pitch case. However, amplitude growth ceases at later time. • Decrease pitch:slender helical density wrapped by B-field developed. Amplitude growth continues throughout simulation.

  21. Time evolution Volume-averaged kinetic energy transverse to the z-axis Constant density Decrease density tA: Alfven crossing time Solid: constant pitch Dotted: increase pitch Dashed: decrease pitch • Initial exponential linear growth phase and subsequent non-linear evolution • Density Decline: more rapid initial growth and decline(by more gradual radial decline in the Alfven velocity) . • Pitch increase: slower growth • Pitch decrease: more rapid growth • Consistent with non relativistic linear analysis in Appl et al. (2000)

  22. CD kink instability of Sub-Alfvenic Jets:Temporal Properties • At the next stage, we investigate the influence of jet shear motions on the stability and nonlinear behavior of CD kink instability. • We consider sub-Alfvenic jets because this configuration is stable against KH instability. • Only focus on CD kink instability at this work.

  23. Initial Condition Mizuno et al. 2010, ApJ, submitted • Cylindrical sub-Alfvenic jets (vj=0.2c) with force-free helical magnetic field (stable against KH instability) • Magnetic pitch (P=RBz/Bf): constant, increase, decrease • Density profile: decrease (r=r0 B2) • Jet radius: Rj=1/2a, a, 2a, 4a • Numerical box:-2L < x, y < 2L, 0 < z < 3L(Cartesian coordinates:160 x 160 x 120 zones) • Boundary: periodic in axial (z) direction • Small radial velocity perturbation with m=1(-1) andn=1(-1) modes

  24. Initial Force-Free Configuration Solid: constant pitch Dashed: decrease pitch Jet position

  25. Time evolution of 3D structure • Vj=0.2c, Rj=2a, constant pitch • Similar to static case, displacement of the initial force-free helical field leads to a helically twisted magnetic filament around the density isosurface by CD kink instability • From transition to non-linear stage, helical twisted structure is propagates along jet axis with continuous increase of kink amplitude. Color: density White line: magnetic field lines Vectors: velocity

  26. Dependence on Jet Radius Volume-averaged kinetic and magnetic energies Red: Rj=1/2a, Orange: Rj=a, Green: Rj=2a, Blue: Rj=4a, Black: no jet • Initial exponential linear growth phase and subsequent non-linear evolution similar to static (no jet) case • Larger jet radius: slower linear growth with larger maximum amplitude by jet shear effect • Far from characteristic radius, Rj >> a: jet shear effect becomes weaker and approached to static case • (static case = rigidly moving flow seen in jet frame)

  27. Dependence on Jet Radius 3D helical structure • No difference in helical kink structure • Rj ~ a: flow follows helical kink structure • Rj > a: keep initial straight jet flow even in nonlinear stage (= rigidly moving flow)

  28. Maximum density position at z=8a Propagation of Helical Structure Red: Rj=1/2a, Orange: Rj=a, Green: Rj=2a, Blue: Rj=4a, Black: no jet Rj=2a case • Rj > a: clearly shownthe propagation of helical structure along jet. • larger jet radius: faster propagation speed (~ Vj) . • Propagation speed is decreasing with time.

  29. CD kink instability of Sub-Alfvenic Jets:Spatial Properties Mizuno et al. 2010, in preparation Initial Condition • Cylindrical sub-Alfvenic jet established across the computational domain with a helical force-free magnetic field (stable against KH instabilities) • Vj=0.2c, Rj=1.0 • Radial profile: Decreasing density with constant magnetic pitch • Jet spine precessed to break the symmetry 3D density with magnetic field lines • Preliminary Result • Precession perturbation from jet inlet produces the growth of CD kink instability with helical density distortion. • Helical structure propagates along the jet with continuous growth of kink amplitude in non-linear phase.

  30. Summary • We have investigated stability properties for KH modes of magnetized spine-sheath relativistic jets by 3D RMHD simulations. • The most important result is that destructive KH modes can be stabilized by the presence of magnetized sheath wind even when the jet is super-Alfvenic flow. • Even in the absence of stabilization, spatial growth rate of destructive KH modes can be reduced by the presence of sheath wind (~0.5c) around a relativistic jet spine (>0.9c)

  31. Summery (cont.) • In CD kink instability, we found the initial configuration is strongly distorted but not disrupted. • The linear growth and nonlinear evolution of the CD kink instability depends on the radial density profile and strongly depends on the magnetic pitch profile • In sub-Alfvenic jet case, developed helical kink structure propagates along jet axis with continuous growth of kink amplitude. • The growth rate of CD kink instability and propagation speed of helical kink structure depend on the radius of jet shear boundary.

  32. Future works • Coupling of CD kink/KH instabilities of super-Alfvenic jets • Temporal and spatial properties • Effect of perturbation for Relativistic jet formation • Relation between disk perturbation and formed jet structure • Radiation image/polarization from relativistic jet formation and propagation • Magnetic amplification by relativistic turbulence through relativistic shock propagation • Relativistic magnetic reconnection • Development of resistive relativistic MHD code

  33. Other Research • General relativistic MHD simulations of collapsar as the central engine of GRBs (Mizuno et al. 2004ab) • Development of 3D general relativistic MHD code RAISHIN (Mizuno et al. 2006a) • General relativistic MHD simulations of relativistic jet formation from thin Keplerian disk (Mizuno et al. 2006b, Hardee et al. 2007) • Radiation imaging from BH-accretion disk system (Wu et al. 2008) • MHD effect for relativistic shock and additional jet acceleration (Mizuno et al. 2008, 2009) • (Mizuno et al. 2010 in preparation) • Relativistic Particle-in-Cell simulations of relativistic jets (Nishikawa et al. 2009)

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