WEIBEL, TWO-STREAM, FILAMENTATION, OBLIQUE, BELL, BUNEMAN...WHICH ONE GROWS FASTER?

By A. Bret. 2009

134 citations recorded by the source corpus.

Many competing linear instabilities are likely to occur in astrophysical settings, and it is important to assess which one grows faster for a given situation. An analytical model including the main beam plasma instabilities is developed. The full three-dimensional dielectric tensor is thus explained for a cold relativistic electron beam passing through a cold plasma, accounting for a guiding magnetic field, a return electronic current, and moving protons. Considering any orientations of the wave vector allows to retrieve the most unstable mode for any parameters set. An unified description of the filamentation (Weibel), two-stream, Buneman, Bell instabilities (and more) is thus provided, allowing for the exact determination of their hierarchy in terms of the system parameters. For relevance to both real situations and PIC simulations, the electron-to-proton mass ratio is treated as a parameter, and numerical calculations are conducted with two different values, namely 1/1836 and 1/100. In the system parameter phase space, the shape of the domains governed by each kind of instability is far from being trivial. For low-density beams, the ultra-magnetized regime tends to be governed by either the two-stream or the Buneman instabilities. For beam densities equaling the plasma one, up to four kinds of modes are likely to play a role, depending of the beam Lorentz factor. In some regions of the system parameters phase space, the dominant mode may vary with the electron-to-proton mass ratio. Application is made to solar flares, intergalactic streams, and relativistic shocks physics.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/699032a9c8fe8c61c58c94887868b247a2b8b8d5

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In Astronomy and Astrophysics

1. L. Sironi
2. J. Arons
3. A. Spitkovsky
4. U. Keshet
5. M. Lemoine
6. L. Fletcher
7. D. Giannios
8. E. P. Kontar

In Nuclear and High Energy Physics

1. L. Sironi
2. A. Spitkovsky
3. J. Arons
4. U. Keshet
5. M. Lemoine
6. E. P. Kontar
7. V. Petrosian
8. L. Fletcher

Citations in the corpus

• PARTICLE ACCELERATION IN RELATIVISTIC MAGNETIZED COLLISIONLESS ELECTRON–ION SHOCKS (2010, background): “The compensating current by the incoming electrons triggers the growth of the so-called Bell’s instability, which is expected in this regime of shock parameters (Bret 2009; Lemoine & Pelletier 2010).”
• Relativistic Shocks: Particle Acceleration and Magnetization (2015, background): “A host of micro-instabilities can in principle develop in such anisotropic configurations, see the general discussion by Bret (2009).”
• Recent Advances in Understanding Particle Acceleration Processes in Solar Flares (2011, methodology): “However, lat realization that the resistivity in the reconnection region may be driven to anomalous y high values through the presence of plasma instabilities in the current sheet (see,for xample, Dahlburg et al. 1992; Bret 2009, and references therein).”
• THE MAXIMUM ENERGY OF ACCELERATED PARTICLES IN RELATIVISTIC COLLISIONLESS SHOCKS (2013, background): “4 More precisely, the instability results from the coupling of the electromagnetic filamentation (Weibel) instability with the electrostatic two-stream instability, as explained by Bret (2009).”
• THE COSMOLOGICAL IMPACT OF LUMINOUS TeV BLAZARS. I. IMPLICATIONS OF PLASMA INSTABILITIES FOR THE INTERGALACTIC MAGNETIC FIELD AND EXTRAGALACTIC GAMMA-RAY BACKGROUND (2011, background): “Due to the geometry of the coupled modes, the oblique instability is primarily sensitive to transverse beam-velocity dispersions, though shares the resistance to beam heating with its two-stream cousin (Bret et al. 2005b; Bret 2009; Bret et al. 2010b; Lemoine & Pelletier 2010).”