The remarkable discovery by the Chandra X-ray observatory that the Crab nebula’s jet periodically changes direction provides a challenge to our understanding of astrophysical jet dynamics. It has been suggested that this phenomenon may be the consequence of magnetic fields and magnetohydrodynamic instabilities, but experimental demonstration in a controlled laboratory environment has remained elusive. Here we report experiments that use high-power lasers to create a plasma jet that can be directly compared with the Crab jet through well-defined physical scaling laws. The jet generates its own embedded toroidal magnetic fields; as it moves, plasma instabilities result in multiple deflections of the propagation direction, mimicking the kink behaviour of the Crab jet. The experiment is modelled with three-dimensional numerical simulations that show exactly how the instability develops and results in changes of direction of the jet.
X-ray images from the Chandra X-ray Observatory1,2 show that the South-East jet in the Crab nebula changes direction every few years (Supplementary Fig. 1). This fascinating phenomenon is also seen in jets associated with pulsar wind nebulae and other astrophysical objects3,4,5, and therefore is a fundamental feature of astrophysical jet evolution that needs to be understood6,7,8,9,10,11,12,13. The South-East Crab nebula jet is a highly collimated, mildly relativistic gas outflow from a pole of the rapidly rotating Crab pulsar, confined by a toroidal magnetic field (B) and accelerated outwards initially by means of magnetic fields (Poynting flux) drawing from the pulsar rotational energy6,8,9,10,11,12,13,14,15.
Astrophysical jets can be studied in a controlled environment using appropriately scaled laboratory experiments that reproduce and study critical physical aspects; even though laboratory-generated supersonic plasma jets and astrophysical jets have very different scales, they can have similar dimensionless hydrodynamic and magnetic field parameters (as will be shown below) and therefore can share common physical properties16,17,18. These important similarities allow us to scale our laboratory results to the conditions in the Crab nebula, showing that the laboratory approach provides an incisive platform for studying various properties of astrophysical jets. To mimic the kink behaviour of the Crab jet, a laboratory experiment requires magnetic fields with the right properties: the fields must have a strong azimuthal (toroidal) component generated near the target where the jet is launched, and the fields must be embedded in (‘frozen-in’), and advected with, the fast moving magnetized plasma flow.
The development and use of diagnostics that enable visualization and quantification of magnetic fields and magnetohydrodynamic (MHD) instabilities is as important as the creation of the plasma jet itself. Most conventional plasma diagnostics, using X rays and optical photons, are sensitive to plasma density and temperature but not to electromagnetic fields19,20,21. The recently developed method of monoenergetic proton radiography22 (Methods section) is sensitive to electromagnetic fields and can provide spatial visualization and quantitative measurements.
Here we report experiments using scaled plasma jets, generated by high-power lasers, to reproduce and model the Crab jet (Methods section and Supplementary Fig. 2). Magnetic fields and current-driven MHD instabilities taking place in the jet, visualized and measured directly by monoenergetic proton radiography22, have been unambiguously identified as the mechanisms that cause such a unique jet kink behaviour. We show how the toroidal magnetic field embedded in the supersonic jet triggers plasma instabilities and results in considerable deflections throughout the jet propagation, mimicking the kinks in the Crab jet. We also demonstrate that these kinks are stabilized by high jet velocity, consistent with the observation that instabilities alter the jet orientation but do not disrupt the overall jet structure. Our laser experiments produce plasma jets characterized by higher plasma temperatures (>∼keV) and faster flow velocities (>∼1,000 km s−1) that are at least one to two orders of magnitudes higher (faster) than those achievable by other experimental approaches19,20,21. Our experiments also produce plasma jets that have magnetic Reynolds numbers large enough for the magnetic field to be ‘frozen into’ the plasma flow. Consequently, the plasma in the jet must follow the field topology and its evolution, which is locally kinked but globally ‘collimated’ along the propagation axis. We successfully model these laboratory experiments with a validated three-dimensional (3D) numerical simulation, which in conjunction with the experiments provide compelling evidence that we have an accurate model of the most important physics behind the observed kinking of the Crab nebula jet. These experiments not only advance our knowledge of the structure and dynamics of the Crab jet, but also open up opportunities for laboratory study of jets from a variety of other astrophysical objects.
Laser-driven scaled plasma jet
In our laboratory experiments, we form plasma jets through the collision of expanding, laser-driven plasma plumes (Fig. 1). The laser-foil interaction induces self-generated magnetic fields due to the Biermann battery effects23 (∂B/∂t∝∇ne × ∇Te, where ne and Te are electron density and temperature, respectively) that are predominantly toroidal with respect to each plume and to the jet that is formed from the collision of these plumes (Fig. 1b). The magnetic fields are embedded in and advance with the moving jet (∂B/∂t∝∇ × (vj × B), where vj is jet velocity), mimicking the fundamental scenario that magnetic fields are anchored in the rapidly spinning Crab pulsar and advected with the Crab jet.
Figure 1a shows proton radiographs of the plasma jets at different times, indicating a structure that is collimated throughout its propagation but has a sequence of clumps and changes of direction along its length. These features reflect perturbations in the magnetic field structure around the jet (Fig. 2), and they grow locally and expand at each axial position where the jet is unstable. The shape of the jet is serpentine due to the kink instability, and so can be viewed as comprised of ellipsoidal blobs that are typically viewed with the proton radiography from an angle θ∼45°. Adopting this picture, we can apply the analysis of ref. 24 for ellipsoidal blobs. Interpreting the structures seen in the proton radiography images as caustics, we use the criterion for caustic formation24, which indicates that B>0.8 MG for θ=45°. Shown in Fig. 1d are cartoons illustrating the most feasible and fast growing MHD current-driven instabilities: Mode m=0 (sausage) arises as the Bϕ tension is enhanced by radial contraction, responsible for the axis pinching when |Bϕ|>√2|BP|. Mode m=1 (kink) arises when the strength and pressure of Bϕ increase at the inside of the kinks and decrease outside. |Bϕ||BP|−1λ(2πrj)−1>α, with α=1 is the Kruskal–Shafranov criterion for the kink instability25, where λ is the modulation wavelength and rj the jet radius. In astrophysical jets, effects like expansion can tend to stabilize the jet10, resulting in α larger than but of order unity. This scenario is illustrated by experiment with a flat target (Fig. 3) where the plasma jet is stabilized when magnetic field is overwhelmed by the parallel components as the toroidal components around the jet are too weak to excite the MHD instability. The unstable modes have a growth rate γ comparable to the inverse of the time required for phase velocity of an Alfvén wave (vA=B/√4πρ) to cross the unstable jet column26
Using the measured values rj∼0.5 mm and λ∼0.6–0.7 mm, and vA∼1,000 km s−1 around the jet launching region, we find γ∼3 × 109 s−1, which is consistent with the instability evolution time implied by Fig. 1a.
Modelling of experiments with numerical simulation
To model the observations of the plasma jet, a 3D numerical simulation was performed with the radiation-MHD code FLASH27,28 (Methods section). The simulation was post-processed to provide a more complete physical picture of the jet behaviour, leading to the images in Fig. 4 showing the spatial variations of various quantities at t≈t0+5.0 ns in the plane containing the jet’s axis. Figure 4a shows that a modulated central ‘spine’ (backbone) region with stronger field strength is formed, and is surrounded by asymmetrically distributed, weaker fields around the jet core. When the field is sufficiently large and has nonuniform toroidal components Bϕ, current-driven MHD kink modes are excited with the susceptibility increasing with increasing |Bϕ/BP| (Fig. 4b). Such a structure is confirmed by the corresponding distribution of β=8πnkT/B2 (the ratio of plasma thermal to magnetic pressures) in Fig. 4c: in the jet core β<∼1, showing the flow is magnetically dominated, while in the surrounding plasma β>1. This indicates that the jet is globally collimated due to inertial confinement and magnetic tension, but locally kinked. The jet is not in force-free equilibrium: the gradient of thermal pressure is not in local balance with the sum of magnetic-pressure gradient and magnetic tension (hoop stress −Bϕ2/4πr); that is,
The ‘clumps’ and ‘kinks’ shown in Fig. 4a–c are similar to those we observe in the experiments (Fig. 1a). The distribution of the simulated plasma density depicted in Fig. 4d shows a clear kink structure that is correlated with the field topology in Fig. 4a.
Validation of numerical simulations
The FLASH simulation was used to predict the physical properties of the jet (Methods section). These were compared quantitatively with the experimental measurements, including proton radiography (Fig. 1) and Thomson scattering29 (Supplementary Fig. 3). Figure 5a shows the measured jet positions and velocities which match the simulations well, providing compelling evidence for the validity of the numerical simulation. The velocity at the front of the jet after it has been traveling for several nanoseconds is estimated to be vj∼1,500 km s−1, indicating supersonic jet propagation with an internal Mach number M∼3. Such a high jet velocity has two important effects on jet propagation. First, high Mach numbers suppress the Kelvin-Helmholtz instability, lessening the entrainment of the surrounding plasma in the jet plasma. Second, the high jet velocity helps to move the ‘frozen-in’ non-uniform fields, leading to smoothing of asymmetric magnetic field line distributions, stabilizing the jet. Further validation is provided in Fig. 5b,c, where plasma densities and temperatures measured using Thomson scattering are plotted against the time-resolved jet positions, respectively (Supplementary Fig. 3), and agree well with the numerical simulation. Again, this consistency greatly increases our confidence that the simulation has captured the most important physics in the experiments.
The magnetization parameter (=B2/8πρvj2, the ratio of the jet magnetic to ram pressures) shown in Fig. 6a is σ≥1 near the region where the jet was launched, and ∼10−2–10−3 near the jet head. These values compare very well to those of the Crab nebula, where observations and simulations indicate that σ≥1 close to the pulsar pole where the jet is launched, and σ∼10−2–10−3 near the termination shock where the jet becomes subsonic13. The morphological similarities between the Crab jet (Supplementary Fig. 1) and the laboratory jet can be clearly seen in the simulated current density map (Fig. 6b). The latter reveals kinks, knots, and large-scale radial deflections that are reminiscent of the structures and dynamics observed in the Crab pulsar outflow. This picture of a ‘current-carrying’ jet is in agreement with existing numerical efforts on modelling the Crab jet10,13 and the morphology mimics the jet structures observed in Chandra X-ray imaging1.
These similarities provide rigorous justification of the relevance of the plasma jet to the Crab nebula jet, preserving the facts that the energy flux is predominantly carried by the Poynting flux close to the pulsar pole and by the particles close to the termination shock. The consistency between the experiments and the simulation provides compelling evidence that strong toroidal magnetic fields and the associated MHD kink instabilities are the cause of the observed jet structure, and that the simulation has captured the basic physics behind kink behaviour in jets. Furthermore, this comparison confirms the hypothesis that the observed directional change of the Crab jet can be caused by strong toroidal magnetic fields and associated MHD kink instabilities.
Other evidence of the relevance of our experiments to the jet in the Crab nebula is provided by several important dimensionless parameters. Both jets have a Lorentz factor of the order of unity (Γ=1 for the laboratory plasma jet and Γ≈1.09 for the Crab Nebula jet30). Similarity in the MHD equations requires that the dissipative processes be negligible for both systems. This requirement is met if the viscosity, thermal conduction, and magnetic diffusion terms can be neglected in the momentum, energy, and generalized Ohm’s law equations. Equivalently, a number of corresponding dimensionless numbers, such as the Reynolds number Re(=Lvj/ν, the ratio of inertial forces to viscous force, where L is jet scale size and ν is the kinematic viscosity), the Péclet number Pe(=Lvj/κ, the ratio of heat convection to conduction, where κ is the thermal diffusivity), and the magnetic Reynolds number RMe(=Lvj/Dm, the ratio of flow velocity to diffusion velocity, where Dm is the magnetic diffusivity) must be large in both systems. Table 1 shows that all of these numbers are large, demonstrating that these important conditions are met. Table 1 also lists the other physical parameters and dimensionless numbers that are relevant to this laboratory jet and to the jet in the Crab nebula. To scale the laboratory results to the environment of the Crab nebula, the MHD equations need to be invariant under the transformations given below for the two systems17,18:
where the subscripts ‘lab’ and ‘crab’ refer to the laboratory and Crab nebula jets, respectively. As shown in Table 1, excellent MHD scaling is obtained with a∼1.6 × 10−20, b∼1.7 × 1025 and c∼1.1 × 1019.
In summary, our scaled laboratory experiments and validated numerical simulation reveal that the change in direction observed in the Crab jet can be attributed to magnetic fields and the associated MHD kink instabilities. This work not only advances our knowledge of such jet structure and dynamics, but also opens up tremendous opportunities in the laboratory to explore jets from a variety of other astrophysical objects, including active galactic nuclei, young stellar objects, X-ray binary systems and pulsar wind nebulae.
In our experiment, performed at the OMEGA Laser Facility31 and illustrated schematically in Supplementary Fig. 2, the plasma jet was generated by the interaction of laser beams with a special target. The target was constructed with two 50-μm-thick, 3 × 3 mm plastic (CH) foils separated by 60°. Each individual foil was driven by two laser beams (0.351 μm in wavelength) at an angle ∼28° to the foil normal, with total energy ∼1,000 J in a 1-ns, square-top laser pulse with full spatial and temporal smoothing. The laser spot has a diameter of ∼850 μm determined by phase plate SG4 (defined as 95% energy deposition), resulting in a laser intensity of order of ∼2 × 1014 W cm−2. Laser ablation generated a plasma plume on each foil, and the collision of these plumes forms a high Mach number plasma jet that propagates into the OMEGA chamber32. During laser illumination and heating, ∼Megagauss B fields (predominantly toroidal) are generated around each expanding, hemispherical plasma plume because of the Biermann battery effect23 due to non-collinear electron density and temperature gradients (∇ne × ∇Te). The collision of the plasma plumes with B fields of opposing sign eventually results in magnetic reconnection, leading to the formation a new magnetic topology with strong toroidal fields around the plasma jet32.
Monoenergetic proton radiography22 has been developed on the OMEGA laser facility and utilized for backlighting of laser-produced plasma jets. From the Lorentz force (FL=q(E+v × B)), deflections due to magnetic fields can be estimated as:
where a(=1 cm) and A(=28 cm) are distances from backlighter to the subject target and to the detector in this experiment, respectively; mp is the proton mass and Vp is the proton velocity; q is the proton electric charge, ξ is the proton deflection distance and dl is the differential pathlength along the proton trajectory. This technology22 consists of a monoenergetic proton backlighter source and a matched imaging detector.
The backlighter is formed by an exploding-pusher implosion with a D3He- (deuterium-helium-3) filled, glass-shell capsule22 driven by 16–30 of the 60 OMEGA laser beams31. The capsule has a typical diameter ∼420 μm and shell thickness ∼2 μm, filled with 18 atm of equimolar D3He gas. The laser delivered ∼10 kJ in a 1 ns square pulse. Supplementary Table 1 summarizes the characteristics of the typical backlighter used in these experiments. The timing of the backlighter implosions was adjusted to provide radiographic images at different times relative to when the lasers turned on. The detection system33 consists of a layered assembly of metallic foils and solid-state nuclear track detector CR-39 on which backlighting protons are recorded at 100% efficiency. The CR-39 has a chemical composition of C12H18O7. When a charged particle passes through CR-39, it leaves a trail of damage along its track in the form of broken molecular chains and free radicals. The amount of local damage along the track is related to the local rate at which energy is lost by the particle. In particular, since dE/dx is different for protons at different energies, protons with different energies result in different track diameters. In this experiment, the CR-39 is etched for 2–3 h in a 6N solution of NaOH, which reveals the tracks with diameters on the order of ∼10 μm. An automated microscope system scans and records information about the protons tracks, including their location on the piece of CR-39. Custom software is used to determine track properties and to transform that information into an image of proton fluence incident on the CR-39.
3D numerical simulation
The 3D Cartesian radiation-MHD simulation of the experiment was performed using FLASH27,28,34, a publicly available, multi-physics, finite-volume, shock-capturing code27. The simulation takes advantage of the full range of HEDP capabilities of the code, so as to accurately model the physical processes in play. The MHD equations are evolved using a directionally unsplit staggered mesh solver35, extended to three temperatures36, adding also the Biermann battery effect23,37,38. We include non-ideal effects such as explicit Spitzer resistivity, implicit thermal conduction and heat exchange, as well as multi-group radiation diffusion with multi-material tabulated opacities and equations of state. The laser energy deposition is accurately modelled using a 3D optical ray trace laser package39.
The computational domain spans 0.5 cm in X and Y, and 1 cm in Z (Supplementary Fig. 4), and is discretized on ∼3.3 × 107 zones (∼20 μm cell size). The reconstruction is carried out with a Piecewise Parabolic Method40, employing a minmod limiter. The Godunov fluxes are recovered with an HLLC (Harten, Lax and van Leer-Contact)41 Riemann solver. Outflow boundary conditions are imposed on all sides. The experimental target is modelled as two 3 × 3 mm polystyrene foils at a density of 1.04 g cm−3 and room temperature with an angle of 60° between them. A 3ω laser beam (comprised of 1.6 × 104 rays) with a 1 ns square pulse profile and 1 kJ of energy illuminates each of the two foils. The incidence angle and the SG8 phase plates (with very similar characteristics to the SG4 plates used in the experiment) determine the spot size and shape for each beam. The beams point at the center of the foils, albeit one of the beams is offset by ∼100 μm in the Z direction towards the target’s base to introduce an asymmetry that excites the m=1 (kink) mode. Conversely, we introduce a small-amplitude, time-dependent, sinusoidal perturbation13,42 on the transverse velocity components in the interaction region where the jet is formed, so as to excite the m=0 (sausage) mode. The amplitude of the perturbation is 1% of the flow speed, with a period=0.1 × τ=0.1 ns, where τ is the system’s timescale. The evolution of the system is followed for 5 ns.
The authors declare that the data supporting the findings of this study are available within the article and its Supplementary Information files, and are available from the authors on request. The FLASH code is publicly available through the webpage of Flash Center, University of Chicago (flash.uchicago.edu).
How to cite this article: Li, C. K. et al. Scaled laboratory experiments explain the kink behaviour of the Crab Nebula jet. Nat. Commun. 7, 13081 doi: 10.1038/ncomms13081 (2016).
We thank the OMEGA operations and target fabrication crews for their assistance in carrying out these experiments and R. Frankel, and E. Doeg for their help in processing of CR-39 data used in this work. The experiments were supported in part by US DOE (Grant No. DE-FG03-09NA29553, No.DE-SC0007168), LLE (No.414090-G), NLUF (No.DE-NA0000877), FSC (No.415023-G) and LLNL (No. B580243). Numerical simulations were supported in part by the US DOE NNSA ASC under Field Work Proposal No. 57789 to the Argonne National Laboratory, and by NIH through resources provided by the Computation Institute and the Biological Sciences Division of the University of Chicago and Argonne National Laboratory (Grant 1S10OD018495-01). Partial support from the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreements no. 256973 is acknowledged. The software used in this work was developed in part by the DOE NNSA ASC- and DOE Office of Science ASCR-supported Flash Center for Computational Science at the University of Chicago. This research used resources from the Director’s Discretionary Program of the Argonne Leadership Computing Facility, supported by DOE Office of Science User Facility (DE-AC02-06CH11357).
The structure and evolution of self-generated magnetic fields associated with plasma jet, simulated with 3D hydrodynamic code FLASH, illustrating how the colliding plasma plumes create a modulated central "spine" (backbone) region with strong magnetic fields that is surrounded by asymmetricallydistributed weaker fields. The movie clearly indicates the kink generation and advection of jet magnetic fields.
The structure and evolution of |Bt| to |BP| ratio in plasma jet, simulated with 3D hydrodynamic code FLASH, providing spatially and temporally resolved field distribution. The movie shows that if the field is sufficiently large and has a non-uniform toroidal component Bf, current-driven MHD kink modes are excited with the susceptibility of this happening increasing with increasing |Bϕ/BP|.
The structure and evolution of thermal beta associated with plasma jet, simulated with 3D hydrodynamic code FLASH, revealing how the kinks are generated. The movie indicates that in the jet core, β< ∼1, while in the surrounding plasma, β >1, illustrating that the jet is globally collimated due to inertial confinement and magnetic tension, but locally kinked.
The structure and evolution of jet plasma density, simulated with 3D hydrodynamic code FLASH. The movie shows that the magnetic Reynolds number in the experiment is large enough for the magnetic field to be "frozen into" the plasma flow. Consequently, the plasma in the jet must follow the field topology and its evolution, which is locally kinked but globally "collimated' along the propagation axis.
The structure and evolution of the magnetization parameter associated with plasma jet, simulated with 3D hydrodynamic code FLASH. The movie provides justification of plasma jet relevant to the Crab jet and the critical similarities preserve the facts that the energy flux is predominantly carried by the Poynting flux close to the pulsar pole and by the particles close to the termination shock.
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