Multidimensional electron beam-plasma instabilities in the relativistic regime

Bret, Antoine; Grémillet, L.; Dieckmann, Mark E

doi:10.1063/1.3514586

Cited by 232 publications

(306 citation statements)

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“…The kinetic oblique mode is indeed resposible for the peak in the electric field energy observed at ω e t ∼ 1000 in Figure 1(a) (red and blue lines), which produces a moderate increase in the fraction of beam energy transferred to the background electrons (orange line in Figure 1(a) at ω e t ∼ 1000). In this phase, the 2D structure of the longitudinal electric field in Figure 1 As expected, the increase in the transverse momentum dispersion has suppressed the modes having k ⊥ k , which are most sensitive to transverse temperature effects (e.g., Bret et al 2010b).…”

Section: Resultsmentioning

confidence: 99%

“…Since the oblique mode is heating up the beam in the transverse direction (solid blue line in Figure 1(b)), the exponential growth at the reactive rate ω OBL will necessarily terminate, when the assumption of a cold beam required by the reactive approximation becomes invalid. It is well known that the system will transition from the reactive phase to the kinetic phase when the beam velocity dispersion ∆v b reaches (e.g., Fainberg et al 1970;Bret et al 2010b)…”

Section: Resultsmentioning

confidence: 99%

“…As they stream through the IGM plasma, the electron-positron pairs are expected to trigger collective plasma instabilities (as opposed to binary Coulomb collisions, that are negligible, as discussed by Miniati & Elyiv 2013). For the parameters relevant to blazar-induced beams (i.e., dilute and ultra-relativistic), the fastest growing mode is the electrostatic oblique instability (e.g., Fainberg et al 1970;Bret et al 2010b), whose linear growth rate can exceed the IC cooling rate by several orders of magnitude . Assuming that the instability keeps growing at the linear rate until all the beam energy is deposited into the IGM, the beam energy loss will be dominated by collective beam-plasma instabilities, rather than IC cooling.…”

Section: Introductionmentioning

confidence: 99%

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RELATIVISTIC PAIR BEAMS FROM TeV BLAZARS: A SOURCE OF REPROCESSED GeV EMISSION RATHER THAN INTERGALACTIC HEATING

Sironi

Giannios

2014

ApJ

100

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The interaction of TeV photons from blazars with the extragalactic background light produces a relativistic beam of electron-positron pairs streaming through the intergalactic medium (IGM). The fate of the beam energy is uncertain. By means of two-and three-dimensional particle-in-cell simulations, we study the non-linear evolution of dilute ultra-relativistic pair beams propagating through the IGM. We explore a wide range of beam Lorentz factors γ b 1 and beam-to-plasma density ratios α 1, so that our results can be extrapolated to the extreme parameters of blazarinduced beams (γ b ∼ 10 6 and α ∼ 10 −15 , for the most powerful blazars). For cold beams, we show that the oblique instability governs the early stages of evolution, but its exponential growth terminates -due to self-heating of the beam in the transverse direction -when only a negligible fraction ∼ (α/γ b ) 1/3 ∼ 10 −7 of the beam energy has been transferred to the IGM plasma. Further relaxation of the beam proceeds through quasi-longitudinal modes, until the momentum dispersion in the direction of propagation saturates at ∆p b, /γ b m e c ∼ 0.2. This corresponds to a fraction ∼ 10% of the beam energy being ultimately transferred to the IGM plasma, irrespective of γ b or α. If the initial dispersion in beam momentum satisfies ∆p b0, /γ b m e c 0.2 (as typically expected for blazar-induced beams), the fraction of beam energy deposited into the IGM is much smaller than ∼ 10%. It follows that at least ∼ 90% of the beam energy is still available to power the GeV emission produced by inverse Compton up-scattering of the Cosmic Microwave Background by the beam pairs.

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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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RELATIVISTIC PAIR BEAMS FROM TeV BLAZARS: A SOURCE OF REPROCESSED GeV EMISSION RATHER THAN INTERGALACTIC HEATING

Sironi

Giannios

2014

ApJ

100

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“…In contrast to standard geometry implicated in WI, recent theoretical studies of Bret (2009, Bret, Gremillet & Dieckman (2010) have also shown the importance of oblique modes.…”

Section: Introductionmentioning

confidence: 99%

Vlasov models for kinetic Weibel-type instabilities

2017

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The Weibel instability, driven by a temperature anisotropy, is investigated within different kinetic descriptions based on the semi-Lagrangian full kinetic and relativistic Vlasov-Maxwell model, on the multi-stream approach, which is based on a Hamiltonian reduction technique, and finally, with the full pressure tensor fluid-type description. Dispersion relations of the Weibel instability are derived using the three different models. A qualitatively different regime is observed in Vlasov numerical experiments depending on the excitation of a longitudinal plasma electric field driven initially by the combined action of the stream symmetry breaking and weak relativistic effects, in contrast with the existing theories of the Weibel instability based on their purely transverse characters. The multi-stream model offers an alternate way to simulate easily the coupling with the longitudinal electric field and particularly the nonlinear regime of saturation, making numerical experiments more tractable, when only a few moments of the distribution are considered. Thus a numerical comparison between the reduced Hamiltonian model (the multi-stream model) and full kinetic (relativistic) Vlasov simulations has been investigated in that regime. Although nonlinear simulations of the fluid model, including the dynamics of the pressure tensor, have not been carried out here, the model is strongly relevant even in the three-dimensional case.

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“…7,11 The instability is driven by a thermal anisotropy of a single electron distribution rather than by counterstreaming electron beams 12 and is thus similar to the Weibel instability in its original form. [13][14][15][16][17] It is the result of the electron's slowdown by the ambipolar electrostatic field, which is sustained by the plasma density gradient of the rarefaction wave.…”

Section: Introductionmentioning

confidence: 99%

Magnetic instability in a dilute circular rarefaction wave

2012

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Observation of parametric instabilities in the quarter critical density region driven by the Nike KrF laser Phys. Plasmas 20, 022701 (2013) Magnetic stochasticity and transport due to nonlinearly excited subdominant microtearing modes Phys. Plasmas 20, 012307 (2013) Dynamic stabilization of Rayleigh-Taylor instability: Experiments with Newtonian fluids as surrogates for ablation fronts Phys. Plasmas 20, 012706 (2013) Decay instability of an upper hybrid wave in a magnetized dusty plasmas Phys. Plasmas 20, 013706 (2013) A simple class of singular, two species Vlasov equilibria sustaining nonmonotonic potential distributions Phys. Plasmas 20, 012107 (2013) The growth of magnetic fields in the density gradient of a rarefaction wave has been observed in simulations and in laboratory experiments. The thermal anisotropy of the electrons, which gives rise to the magnetic instability, is maintained by the ambipolar electric field. This simple mechanism could be important for the magnetic field amplification in astrophysical jets or in the interstellar medium ahead of supernova remnant shocks. The acceleration of protons and the generation of a magnetic field by the rarefaction wave, which is fed by an expanding circular plasma cloud, is examined here in form of a 2D particle-in-cell simulation. The core of the plasma cloud is modeled by immobile charges, and the mobile protons form a small ring close to the cloud's surface. The number density of mobile protons is thus less than that of the electrons. The protons of the rarefaction wave are accelerated to 1/10 of the electron thermal speed, and the acceleration results in a thermal anisotropy of the electron distribution in the entire plasma cloud. The instability in the rarefaction wave is outrun by a TM wave, which grows in the dense core distribution, and its magnetic field expands into the rarefaction wave. This expansion drives a secondary TE wave. V C 2012 American Institute of Physics. [http://dx

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Multidimensional electron beam-plasma instabilities in the relativistic regime

Cited by 232 publications

References 237 publications

RELATIVISTIC PAIR BEAMS FROM TeV BLAZARS: A SOURCE OF REPROCESSED GeV EMISSION RATHER THAN INTERGALACTIC HEATING

RELATIVISTIC PAIR BEAMS FROM TeV BLAZARS: A SOURCE OF REPROCESSED GeV EMISSION RATHER THAN INTERGALACTIC HEATING

Vlasov models for kinetic Weibel-type instabilities

Magnetic instability in a dilute circular rarefaction wave

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