Multidimensional simulations of magnetic field amplification and electron acceleration to near-energy equipartition with ions by a mildly relativistic quasi-parallel plasma collision.

Multidimensional simulations of magnetic field amplification and electron acceleration to near-energy equipartition with ions by a mildly relativistic quasi-parallel plasma collision.

Gareth C. Murphy, Mark E. Dieckmann, and Luke O’C. Drury Manuscript received December 1, 2009; revised July 12, 2010; accepted July 26, 2010. This work was supported in part by the Science Foundation Ireland under Grant 08/RFP/PHY1694 and in part by the Swedish Vetenskapsrådet.G. C. Murphy and L. O’C. Drury are with the Dublin Institute for Advanced Studies, Dublin 2, Ireland (e-mail: gmurphy@cp.dias.ie; ld@cp.dias.ie).M. E. Dieckmann is with the Department of Science and Technology, Linkšping University, 60174 Norrkp̈ing, Sweden (e-mail: Mark.E. Dieckmann@itn.liu.se).Color versions of one or more of the figures in this paper are available online at http://ieeexplore.ieee.org.Digital Object Identifier 10.1109/TPS.2010.2063442
Abstract

The energetic electromagnetic eruptions observed during the prompt phase of gamma-ray bursts are attributed to synchrotron emissions. The internal shocks moving through the ultrarelativistic jet, which is ejected by an imploding supermassive star, are the likely source of this radiation. Synchrotron emissions at the observed strength require the simultaneous presence of powerful magnetic fields and highly relativistic electrons. We explore with one and three-dimensional relativistic particle-in-cell simulations the transition layer of a shock, that evolves out of the collision of two plasma clouds at a speed 0.9c and in the presence of a quasi-parallel magnetic field. The cloud densities vary by a factor of 10. The number densities of ions and electrons in each cloud, which have the mass ratio 250, are equal. The peak Lorentz factor of the electrons is determined in the 1D simulation, as well as the orientation and the strength of the magnetic field at the boundary of the two colliding clouds. The relativistic masses of the electrons and ions close to the shock transition layer are comparable as in previous work. The 3D simulation shows rapid and strong plasma filamentation behind the transient precursor. The magnetic field component orthogonal to the initial field direction is amplified in both simulations to values that exceed those expected from the shock compression by over an order of magnitude. The forming shock is quasi-perpendicular due to this amplification. The simultaneous presence of highly relativistic electrons and strong magnetic fields will give rise to significant synchrotron emissions.

Plasma accelerators, Plasma simulation, Plasma transport processes, Magnetic confinement

Mildly relativistic plasma collisions are commonly found in astrophysical scenarios, in particularly strong supernovae [1, 2, 3, 4], in gamma ray bursts (GRBs) [5, 6, 7, 8] and

in the jets of microquasars [9, 10, 11] and active galactic nuclei [12] [13] [14].

The prompt emissions of the ultrarelativistic GRBs are probably the most spectacular eruptions of electromagnetic radiation in the universe, as they are observed across cosmological distances. Since the first observations of GRBs thousands have been detected. They all share a common signature of energetic radiation attributed to highly relativistic electrons and strong magnetic fields.

The details of the underlying physical mechanism which causes the prompt emissions is still unknown. In particular, the method by which magnetic field is generated and sustained, and the means by which electrons are accelerated to ultrarelativistic speeds in sufficient numbers to be injected into the Fermi mechanism is still under debate. It is therefore interesting and relevant to use numerical simulations to probe the behaviour of magnetised shocks to see if a robust mechanism to amplify the field self-consistently may be found.

While the first-order Fermi acceleration mechanism is certainly capable of accelerating particles [15] to ultrarelativistic energies, it requires a seed population of non-thermal particles before it can viably accelerate them to high energies. This mechanism may also not be able to provide rapidly enough the huge quantities of highly relativistic electrons, which drive the prompt emissions of gamma ray bursts. Plasma instabilities driven by the relativistic flow may be a more likely candidate mechanism.

-a Plasma Instabilities

Many instabilities, such as the two-stream, filamentation or Weibel-type and oblique instabilities are expected to operate in the relativistic plasma, and it is not a straightforward task to distinguish the dominant mode [16],[17]. The Weibel-type filamentation instability is expected to generate or amplify magnetic fields. Since the pioneering studies of the electromagnetic Weibel instability [18, 19] and of the beam-Weibel or filamentation instability [20, 21, 22] much work has been done, both analytical [23, 24, 25, 26] and numerical using kinetic particle-in-cell simulations [27, 28, 29] and Vlasov simulations [30].

Reconnection in pair plasmas also excites the Weibel instability [31, 32].

Three-dimensional simulations have the best chance to approximate the correct physics, however they are extremely challenging even for contemporary state of the art supercomputers. It is thus customary to reduce the ion to electron mass ratio, to consider only leptonic flows or to extract aspects of the physically correct three-dimensional plasma behaviour and to model them in 1D or 2D grids at the appropriate spatio-temporal resolution. Certain instabilities can be examined in such reduced geometries like the electrostatic two-stream instability in one dimension and the filamentation instability in two dimensions.

-B Previous related work on plasma collisions and shock formation

Early work was done with counterstreaming and interpenetrating electron-positron plasmas, finding filamentation growing[28][33]. Previous simulation studies of relativistic shocks in more than one spatial dimensions have focussed on mildly to highly relativistic collision speeds and on symmetric clouds of positron-electron pair plasmas[34] [35][36][37]. These simulations are fast, because they only involve one spatiotemporal scale, namely the leptonic one. However these scenarios necessarily exclude the wealth of wave modes and nonlinear processes which exist in ion-electron collisions, due to the mass asymmetry and the massive kinetic energy of the ions. Relevant PIC simulations are the 3D simulation with a low mass ratio discussed in Ref. [38] and the 2D simulation with a high mass ratio performed in Ref. [39]. Magnetic field effects on the collision of two plasma clouds have been investigated too [40].

In this paper we consider the simultaneous effects of a high plasma temperature, a quasi-parallel magnetic field and an initial density asymmetry on the plasma collision. A density asymmetry has been introduced before [38], but here we increase the density ratio from 3 to 10. This high ratio implies, that the initial spectrum of unstable waves should shift from the electromagnetic filamentation instability to the partially electrostatic oblique mode instability [41]. This shift is further emphasized by the high temperature and the guiding magnetic field, which both reduce the growth rate of the filamentation instability compared to those of the other waves. Section 1 provides a more detailed overview over the simulation code and the initial conditions. One-dimensional PIC simulations with a similar setup have been considered first by Ref. [42]. They have been extended to two dimensions, albeit over a limited spatio-temporal range, by Ref. [43]. The 1D PIC simulation data we present here in Section 2 employs a setup that is practically identical to that in Ref. [43] apart from the different ion to electron mass ratio and code. The simulation results are essentially the same, which is clear evidence for the actual physical equipartition of the electron and ion energy in the resulting shock. Obtaining this result only for one mass ratio may be a coincidence. The 3D numerical simulation also presented in Section 2 extends the 2D simulation in Ref. [43], confirming that the front of the dense cloud is practically planar. The 1D PIC simulation is thus at least initially a good approximation for the plasma dynamics close to the front of the expanding dense cloud. However, the plasma density distribution clearly evidences a filamentation behind this front, which is not revealed to this extent by the electromagnetic fields in Ref. [43].

I Initial conditions and numerical Method

Two plasma clouds collide in the simulation box. The species 1 and 2 are the electrons and ions of the dense cloud, while the electrons and ions of the tenuous cloud are the species 3 and 4. The species number gives the subscript of the density . Each cloud has electrons and ions with the mass ratio , with the same density ( and ), temperature and mean speed. Each cloud is thus initially charge- and current neutral. The mean velocity vectors of both clouds point along opposite -directions and they have the same modulus . Each cloud occupies initially one half of the simulation box and their contact boundary is located at at the time . Both clouds are uniform along the directions. No particles are introduced at the boundaries for . The clouds thus detach instantly from the walls and we can use periodic boundary conditions in all directions. A guiding magnetic field gives an electron gyrofrequency that equals the electron plasma frequency of the dense cloud. The is quasi-parallel to the flow (x) direction and at the and . The convection electric field changes its sign across the collision boundary. The collision speed and the electron thermal velocity for 131 keV is c/2. We express space and time in the relevant units of the dense ions (species 2), which are the ion skin depth with and the inverse ion plasma frequency .

We use the particle-in-cell method described in detail in Ref. [44]. The normalised equations are

(1)
(2)
(3)
(4)
(5)
(6)
(7)

The particle of species has the mass . The quantities in SI units (subscript ) can be obtained by the substitutions , , , , and .

The simulation resolution is as follows. For the 1D simulation we use 18,000 cells along and 250 particles per cell. For the 3D simulation we can only simulate a small fraction of the 1D domain with regard to , but we get instead a view of the early 3D filament formation. We use 20 particles per cell and a 3D box composed of 1500x100x100 cells, which spans a total of and a long direction aligned with . The timesteps for the 1D and 3d simulations are both The physical and simulation parameters are summarized in Tables I and II.

Parameter Value
Thermal Velocity
Collision Speed
Beam Speed
Temperature 131 keV
Mass ratio 250
Field Angle 0.1 radians
Density Ratio 10
TABLE I: Physical Parameters
Parameter 1D 3D
No. particles/cell 250 20
No. Cells 18000
Timestep 8.6e-2 8.6e-2
TABLE II: Numerical Parameters

Ii Results

Ii-a One-dimensional simulation

Fig. 1: Left Panel: Electron phase space density . Right Panel: Ion phase space density . The colour scale is 10-logarithmic and the density is expressed in units of a computational particle of the tenuous cloud.

Fig. 2: The Energetic Electromagnetic Structure in 1D: Plots of electric and magnetic field strengths. The upper panel shows the components of and the lower those of .

A circularly polarized electromagnetic wave grows practically instantly at the contact boundary of both clouds and in both simulations. This collision boundary evolves due to the plasma counterstream into a cloud overlap layer. The magnetic field is frozen-in into each cloud outside the overlap layer. Inside this layer, the magnetic field continues to be practically at rest in the reference frame of the dense plasma cloud. The tenuous cloud moves at a mildly relativistic speed relative to this reference frame and the particles are deflected by . The ions and electrons react differently to and, due to its obliqueness, the particles are forced onto an orbit that involves all components of . This corkscrew orbit is discussed in more detail elsewhere [43]. The resulting net current amplifies the magnetic field perturbation and a circularly polarized localized wave structure forms.

Figure 1 displays the most relevant phase space distributions. These are the electron distribution and the ion distribution . The electron distribution reveals the peak energies reached by the electrons, while the ion distribution can reveal the formation of a shock. This is achieved, when the ion distributions of both clouds mix in this phase space projection. The 1D simulation stops at the time , just before the shock formation. The electron distribution demonstrates that the electrons of the tenuous cloud (species 3) are forced onto a strong oscillation, which resembles a corkscrew orbit by the rotation in the -plane. They reach a peak at . The electrons of the dense cloud (species 1), on the other hand, are not yet accelerated on this scale. The electrons of both clouds show a two-stream configuration in the interval . The electrons would drive the oblique mode instability, which is here suppressed by the 1D geometry. Only the electrostatic two-stream instability can develop here and it results in the thermalization of the electrons of the tenuous cloud. This thermalization results in the hot electron population with and with . The phase speed of the two-stream waves is close to the beam speed of the tenuous beam and only those interact resonantly with this wave. The electron phase space distribution of the dense cloud thus remains practically unchanged. The ion phase space distribution reveals that a shock is about to form at . The circularly polarized energetic electromagnetic structure (EES) is here strong enough to force the ions onto a corkscrew orbit. In particular the ions of the tenuous cloud (species 4) are perturbed within the cloud overlap layer. The beam striation in the plane implies, that the associated fields must be at least partially electrostatic. Electrostatic fields and such phase space striation are reminiscent of the Buneman instability, which would develop here between the ions of the tenuous cloud and the electrons of the dense one [45].

Figure 2 displays the distributions of all components of and near the front of the dense cloud at the time , which corresponds to the particle distribution in Fig. 1. The upper panel shows that all components of have reached a comparable strength. The electromagnetic and are phase-shifted by . The magnetic components (lower panel) also show this phase shift. We find that . The must remain constant in a 1D simulation by and a change of in time could only be driven by , which is not possible in 1D. The asymmetry in space of the EES relative to its amplitude maximum may reflect the varying plasma skin depth across the collision boundary. The skin depth is reduced by a factor in the dense plasma. If the penetration depth of the EES is a few ion skin depths, then the wave envelope must decrease more quickly as it enters the dense plasma.

The electrostatic component, is strong in the interval where the electromagnetic fields ( and ) are strong. The electromagnetic fields are tied to the circularly polarized wave structure, which provides the dissipation of the flow energy. The is such, that electrons are accelerated to the left within . This electric field must develop between the ions and the electrons of the tenuous cloud, because the dense cloud in Fig. 1 has not propagated yet that far. The likely cause is the deflection of the electrons of species 3 by the EES. A mere rotation of the electron velocity vector away from the direction, would decrease their flow velocity along . The ion speed remains practically unaffected and an electric charge builds up. The charge results in an electrostatic field, which drags the electrons with the ions. The electrons are accelerated at the expense of the ion kinetic energy. This explains the decrease of the flow speed modulus of the ions of the tenuous cloud and the electron acceleration in this interval.

The EES at the front of the dense cloud has a wavevector parallel to and it can thus be resolved by the 1D simulation. The electromagnetic instabilities in the cloud overlap layer, e.g. the filamentation- and the oblique mode instability, cannot develop here, because their wavevectors are orthogonal or oblique to the beam velocity vector. The plasma dynamics in the cloud overlap layer can thus not be accurately resolved by the 1D simulation, which overemphasizes the importance of the electrostatic two-stream and Buneman instabilities with their flow-aligned wavevectors. We turn to the 3D simulation, with which we can resolve the full wave spectrum during the first few inverse ion plasma frequencies.

Ii-B Three-dimensional plasma filament structure

Fig. 3: Three-dimensional rendering of a simulation of plasma collision. Two isosurfaces of logarithm of ion density are shown at values of 2.5 and 1.9. The filaments are preferentially aligned along the x axis, gyrating in the y z plane.
Fig. 4: Growth and merging of filaments in 3D: Ion density plots at time and . Filaments, which are characterized through density modulations, have increased in size.

Fig. 5: Electromagnetic energy densities at . The left panels show the energy densities and along the initial flow velocity vector, while the right panels show and orthogonal to the initial flow direction.

The 3D simulation is initialised in the same manner as the 1D simulation, except over a smaller domain along , due to computational contraints. Consequently the simulation is run over the significantly shorter time interval than the 1D simulation with its . This time is also somewhat shorter than the runtime of the 2D PIC simulation in Ref. [43], which ran for about 11 inverse ion plasma frequencies for the mass ratio 400. This previous work examined the electromagnetic wave structures in particular at the front of the dense cloud and the simulation’s end, showing that they have remained planar. Here we do not look at the field topology but at the ion density distribution in the entire simulation box.

Figure 3 shows a 3d rendering of the ion density in our numerical simulation. Clearly the counterstreaming ions in three dimensions quickly form filaments, which result in an amplification of the magnetic field orthogonal to the filament axis. These magnetic fields grow until they saturate through magnetic trapping [20]. The strength of the guiding magnetic field has been selected so as to suppress the filamentation instability and the oblique mode instability driven by the electrons [46] in a spatially uniform two-beam configuration. The magnetic field strength has apparently been insufficient to suppress the filamentation and mixed mode instabilities in the presence of ions and of a spatial nonuniformity. A further increase of the amplitude of would be necessary to achieve this [40], but such a field is probably unrealistic for most astrophysical plasmas. The filaments have a preferential alignment with the initial flow velocity vector. This is not surprising, because the filamentation and oblique mode instabilities yield the growth of a magnetic field through the redistribution of the microcurrents carried by the moving charged particles. These microcurrents are obviously strongest along the mean flow (x) direction.

This preferential alignment of the filaments with the x-direction allows us to obtain insight into the filament thickness with slices in the y,z plane. Their coherence length along the filament axis can be estimated from two-dimensional cross-sections in the x,y plane. In Figure 4 we plot these two dimensional cuts from the 3d simulation at the times and . We clearly see the formation of filaments in the ion density distribution, which we identify through a density modulation. Their characteristic diameter is well below 0.1 ion inertial lengths at and is thus comparable to the electron skin depth of the dense cloud . The filament diameter increases beyond 0.1 ion inertial lengths through the dynamical interaction and the mergers of filaments [47]. This small size suggests that until the main driver of the ion beam filamentation has been the electrons. The cut of the ion distribution in the y,z plane in the right panel of Fig. 4 shows some filaments with a significant density depletion and with a radial cross-section. Examples are the low-density structures at and . These are ion filaments immersed in an almost spatially uniform ion background. The ion density is reduced and the small spatial scale suggests that the ions merely follow the electron density, in order to maintain the quasi-neutrality of the plasma. The electron density can be decreased through a magnetic expulsion of the electrons of one of the clouds. The coherence length in the x,y plane is about an ion skin depth, which is an order of magnitude larger than the filament diameter. Some of these filaments may thus be described well by their cross section in the y,z plane, which neglects changes along . We furthermore find that the spatial separation of these radial filaments is larger than their diameter, which implies that these filaments may not interact magnetically over a limited time interval. An equilibrium might be possible during this time between the filament and the spatially uniform background plasma. This equilibrium may be similar to the Hammer-Rostoker equilibrium for a tenuous relativistic electron beam that crosses a dense electron background [48]. The agreement is not exact. Here the ions react to the electric charge built up by the expulsion of the background electrons from the flux tube and the plasma carries an oblique magnetic field. Both aspects have not been considered by Ref. [48].

Finally we notice from the right panel in Fig. 4 that the filamentation also involves the front of the dense cloud at . This filamentation is fairly weak and its scale is again a fraction of the ion skin depth. This implies that a 1D simulation can not reproduce the exact physics at the cloud front but, at least until , this approximation is fairly accurate. It is interesting that a filamentation was not observed in the 2D simulation in Ref. [43] that covered a longer time interval. Several reasons are possible. Firstly, the higher ion mass in the 2D simulation may have delayed the ion filamentation in the y,z plane with respect to the formation of the EES, which modulates the ions along . Both are competing processes. Secondly, the field distribution was used in Ref. [43] to determine the planarity of the cloud front, while the ion density is considered here. The magnetic field amplification by the filamentation instability is much weaker than that by the EES and it may not be visible. The ion density modulation along y,z can thus more accurately reveal the filamentation than the electromagnetic fields. The electromagnetic fields due to the EES reach a much higher energy density than those due to the filamentation instability also in the 3D simulation, which we show now.

Ii-C The Energetic Electromagnetic Structure (EES) in 3D

The EES acts to accelerate charged particles, it can provide the energy dissipation that enforces the formation of a shock and it may provide a compact location for synchrotron radiation in the shock transition layer. The size scale and the energy density is similar to that detected in the Short Large Amplitude Magnetised Structures (SLAMS), which have been observed both in simulations and in those regions of the Earth’s bow shock, where the ambient magnetic field is quasi-parallel to the shock normal [43][49][50] [51][52].

In Figure 5, we see for the first time in 3d dimensions the EES. We make use of the quasi-planarity of the front of the dense cloud at in Fig. 4 and we integrate the energy densities of the electromagnetic fields along y and z, which reduces the noise levels. The energy densities subdivide naturally into (1) , which is unchanged in a 1D simulation, into (2) and (3) , which would be purely electromagnetic in a 1D simulation and into (4) , which would be electrostatic. This distinction is strictly possible only in 1D, because the derivatives along y and z vanish in the Maxwell’s equations. We expect that initially and due to the planarity of the wave structures this holds also in 3D. All energy densities are normalized to the same value, which is the energy density of .

Already at this early simulation time all energy densites surpass by far the initial magnetic energy density as the front of the dense plasma cloud is crossed from the upstream into the cloud overlap layer. The dominant component is , as in the 1D simulation. It peaks at , which is ahead of the dense cloud. The peak of coincides with this location and both thus belong to the same wave structure. Note that, even if the EES were purely magnetic in its rest frame, the convective electric field would be significant due to its rapid propagation. The three-dimensional simulation facilitates the growth of and its peak energy density, which is an order of magnitude less than that of , is reached at the same position as that of . The in the 3D simulation shows like that of a distribution, which differs strongly from its equivalent in the 1D simulation. It grows steadily as we go from to . The electric field in the 1D simulation peaked where the EES was strongest. We interpret the changed distribution in the following way. Let us assume, that the is driven in 1D entirely by the different deflection of the electrons and the ions of the tenuous cloud. The quasi-neutrality of the plasma of the tenuous cloud can then only be maintained by a flow along x, while a 3D simulation enables also a flow of charges along y and z. This will, in turn, alter the electric field distribution. The apparent consequence is that the disappears within the EES. We may attribute instead the increase of in the 3D simulation to the particle heating. The energy density of the electrostatic fluctuations is proportional to the plasma temperature, if the plasma is in an equilibrium (See [53] and references therein). Evidence for this connection is that and the energy density per degree of freedom is thus similar. Since the electrostatic energy density in a thermal equilibrium is also proportional to the particle mass, it is exaggerated by the low statistical plasma representation by a PIC code. The energy density of the EES is, on the other hand, independent of the mass of a computational particle and determined by the kinetic energy density of the inflowing plasma. We may expect that in reality the electromagnetic energy would far exceed the electrostatic one.

Iii Conclusions

In this paper we presents the results of long term 1D and short-term 3D simulations of plasma collisions. We found that in 1D a strong amplification of the field is found in the foreshock, in excess of that expected from compression alone. Strong circularly polarised electromagnetic waves are generated at the collision boundary. We find that electron are accelerated to ultrarelativistic speeds and that the presence of the EES is confirmed in 3D The quasi-parallel magnetic field fails to suppress the filamentation in three dimensions, which was not detected in 2D fields in previous work, probably obscured in the data due to the large contrast provided by the EES. Ion densities are found to be a much better indicator for current filaments. The three dimensional structure of the EES differs from its one-dimensional model, in particular the parallel electric field is diminished at the collision boundary, and is only excited by electron heating. Filaments are produced with a characteristic width of approximately 0.1 ion inertial lengths and a larger separation between filaments, indicating a possibility for a magnetised Hammer-Rostoker equilibrium. The presence and size of the EES could be critical for the acceleration of matter to high energies in plasma shocks. The simulations show the relevance of three dimensional simulations, even over small physical scales.

The EES is relevant to the problem of the large fields and electron acclerations needed to explain the observations of spectra of Gamma Ray Bursts. The study shows that the EES is stable in 3d and that the magnetic field is amplified in 3D. Comparing other magnetic field amplification mechanisms such as Bell’s instability [54], this mechanism does not require addition of external current, but produces electron accleration to near equipartition speeds and a strongly amplified field self-consistently. Shock compression can also amplify the field but only up to a factor , depending on the value of the ratio of specific heats. In this respect it is an important result.

For future work, we need significantly longer timescales to confirm long-term stability of Energetic Electromagnetic Structure. Two-dimensional simulations are already under way with the goal of estimating the long term evolution of the system at high resolution.

Acknowledgment

The project is supported by Science Foundation Ireland grant number 08/RFP/PHY1694 and by the Swedish Vetenskapsrådet. The authors wish to acknowledge the SFI/HEA Irish Centre for High-End Computing (ICHEC) for the provision of computational facilities and support. The Plasma Simulation Code (PSC) was developed by Hartmut Ruhl at the University Ruhr, Bochum.

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