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• W2024550239 abstract "Cosmic-ray streaming instabilities at supernova shocks are discussed in the quasilinear diffusion formalism which takes into account the feedback effect of wave growth on the cosmic ray streaming motion. In particular, the nonresonant instability that leads to magnetic field amplification in the short wavelength regime is considered. The linear growth rate is calculated using kinetic theory for a streaming distribution. We show that the nonresonant instability is actually driven by a compensating current in the background plasma. The nonresonant instability can develop into a nonlinear regime generating turbulence. The saturation of the amplified magnetic fields due to particle diffusion in the turbulence is derived analytically. It is shown that the evolution of parallel and perpendicular cosmic-ray pressures is predominantly determined by nonresonant diffusion. However, the saturation is determined by resonant diffusion which tends to reduce the streaming motion through pitch angle scattering. The saturated level can exceed the mean background magnetic field." @default.
• W2024550239 created "2016-06-24" @default.
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• W2024550239 date "2009-08-11" @default.
• W2024550239 modified "2023-09-25" @default.
• W2024550239 title "Saturated magnetic field amplification at supernova shocks" @default.
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• W2024550239 doi "https://doi.org/10.1111/j.1365-2966.2009.14872.x" @default.
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