Instabilities of relativistic counterstreaming proton beams in the presence of a thermal electron background

Yalinewich, Almog; Gedalin, M.

doi:10.1063/1.3432722

Cited by 24 publications

(33 citation statements)

References 32 publications

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“…The filaments are also susceptible to the Buneman instability, which leads to the growth of resonant waves parallel to the streaming direction. The oblique and parallel modes are rather electrostatic in nature (Yalinewich & Gedalin 2010;Shaisultanov et al 2012;Stockem et al 2014), which implies that the true nature of the longitudinal and transverse electric fields (i.e., electrostatic or induced) is rather mixed, which is due to several waves growing at the same time, although at different rates (see the Section 3.4). In order to quantify the roles of different types of growing waves in the relativistic counter-steaming plasma in the heating of electrons we separate (Helmholtz decomposition) the electric field into rotational and compressive parts, i.e., E E E c r…”

Section: Net Work Done By the Electric Fieldmentioning

confidence: 99%

“…In particlular, the Weibel instability (Weibel 1959), which causes fast growth of a strong magnetic field at small scales in the anisotropic plasma flow, has received much attention as the main isotropization mechanism leading to the shock transition in free-streaming ejecta from violent astrophysical events (Medvedev & Loeb 1999;Wiersma & Achterberg 2004;Lyubarsky & Eichler 2006;Achterberg & Wiersma 2007;Bret 2009;Yalinewich & Gedalin 2010;Shaisultanov et al 2012;Shukla et al 2012). As the dominant modes of the Weibel instability are less than the ion gyroradius, which renders them inefficient scatterers of ions, the long standing question concerning its role in collisionless shocks has been how well it competes with other mechanisms (e.g., Galeev et al 1964;Blandford & Eichler 1987;Lyubarsky & Eichler 2006).…”

Section: Introductionmentioning

confidence: 99%

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Electron Heating in a Relativistic, Weibel-Unstable Plasma

Kumar

Eichler

Gedalin

2015

ApJ

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The dynamics of two initially unmagnetized relativistic counter-streaming homogeneous ion-electron plasma beams are simulated in two dimensions (2D) using the particle-in-cell (PIC) method. It is shown that current filaments, which form due to the Weibel instability, develop a large-scale longitudinal electric field in the direction opposite to the current carried by the filaments as predicted by theory. This field, which is partially inductive and partially electrostatic, is identified as the main source of net electron acceleration, greatly exceeding that due to magnetic field decay at later stages. The transverse electric field, although larger than the longitudinal field, is shown to play a smaller role in heating electrons, contrary to previous claims. It is found that in one dimension, the electrons become strongly magnetized and are not accelerated beyond their initial kinetic energy. Rather, the heating of the electrons is enhanced by the bending and break up of the filaments, which releases electrons that would otherwise be trapped within a single filament and slow the development of the Weibel instability (i.e., the magnetic field growth) via induction as per Lenz's law. In 2D simulations, electrons are heated to about one quarter of the initial kinetic energy of ions. The magnetic energy at maximum is about 4%, decaying to less than 1% by the end of the simulation. The ions are found to gradually decelerate until the end of the simulation, by which time they retain a residual anisotropy of less than 10%.

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Section: Net Work Done By the Electric Fieldmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Electron Heating in a Relativistic, Weibel-Unstable Plasma

Kumar

Eichler

Gedalin

2015

ApJ

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“…For example, the propagation of photons in two-stream plasma systems is a well studied subject in the context of plasma physics, particularly with regard to the so-called two-stream instabilities [1][2][3], many aspects of which have been studied both analytically and numerically [4][5][6][7][8]. In recent works, similar studies have been carried out for magnetized two-stream plasma systems [9][10][11].…”

Section: Introductionmentioning

confidence: 86%

Neutrino propagation in an electron background with an inhomogeneous magnetic field

Nieves¹,

Sahu²

2018

Eur. Phys. J. C

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We study the electromagnetic coupling of a neutrino that propagates in a two-stream electron background medium. Specifically, we calculate the electromagnetic vertex function for a medium that consists of a normal electron background plus another electron stream background that is moving with a velocity four-vector v μ relative to the normal background. The results can be used as the basis for studying the neutrino electromagnetic properties and various processes in such a medium. As an application, we calculate the neutrino dispersion relation in the presence of an external magnetic field (B), focused in the case in which B is inhomogeneous, keeping only the terms of the lowest order in 1/m 2 W and linear in the B and its gradient. We show that the dispersion relation contains additional anisotropic terms involving the derivatives of B, such as the gradient of k · (v × B), which involve the stream background velocity, and a term of the formk · (∇ × B) that can be present in the absence of the stream background, in addition to a term of the formk · v and the well known termk · B that arises in the constant B case. The derivative-dependent terms are even under a C P transformation. As a result, in contrast to the latter two just mentioned, they depend on the sum of the particle and antiparticle densities and therefore can be nonzero in a C P-symmetric medium in which the particle and antiparticle densities are equal.

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“…From the Vlasov-Maxwell system of equations, the dispersion equation for modes exp(ik · r − iωt) has now been solved considering Dirac's delta distributions functions (Watson et al, 1960), waterbag (Bret et al, 2004 or Maxwell-Jüttner distributions functions . The cold case is worth examining in order to evidence the most interesting relativistic effects.…”

Section: Relativistic Electron Beam-plasma Instabilitiesmentioning

confidence: 99%

Recent progresses in relativistic beam-plasma instability theory

Bret¹,

Dieckmann²,

Grémillet³

2010

Ann. Geophys.

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Abstract. Beam-plasma instabilities are a key physical process in many astrophysical phenomena. Within the fireball model of Gamma ray bursts, they first mediate a relativistic collisionless shock before they produce upstream the turbulence needed for the Fermi acceleration process. While non-relativistic systems are usually governed by flow-aligned unstable modes, relativistic ones are likely to be dominated by normally or even obliquely propagating waves. After reviewing the basis of the theory, results related to the relativistic kinetic regime of the poorly-known oblique unstable modes will be presented. Relevant systems besides the wellknown electron beam-plasma interaction are presented, and it is shown how the concept of modes hierarchy yields a criterion to assess the proton to electron mass ratio in Particle in cell simulations.

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Instabilities of relativistic counterstreaming proton beams in the presence of a thermal electron background

Cited by 24 publications

References 32 publications

Electron Heating in a Relativistic, Weibel-Unstable Plasma

Electron Heating in a Relativistic, Weibel-Unstable Plasma

Neutrino propagation in an electron background with an inhomogeneous magnetic field

Recent progresses in relativistic beam-plasma instability theory

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