2009/01/01 by Martin Lemoine, Guy Pelletier, Arno Vanthieghem +3 · 1 citation
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Classical mechanics #Computational physics #Distribution function #Earth Systems and Cosmic Evolution #Gamma-ray bursts and supernovae #Laser-Plasma Interactions and Diagnostics #Lorentz factor #Lorentz transformation #Mechanics #Microturbulence #Momentum (technical analysis) #Nuclear physics #Physics #Plasma #Political science #Population #Quantum electrodynamics #Quantum mechanics #Rest frame #Scattering #Shock (circulatory) #Shock front #Shock wave #astro-ph.HE #physics.plasm-ph
paper · pdf · doi:10.1103/physreve.100.033210
published as Phys. Rev. E 100, 033210 (2019) · Phys. Rev. E, submitted; 13 pages, 5 figures
openalex publication_date 2009/01/01 · openalex created_date 2016/06/24 · arxiv created 2019/07/25 · arxiv updated 2019/10/02 · openalex updated_date 2026/06/22
In this third paper of a series, we discuss the physics of the population of accelerated particles in the precursor of an unmagnetized, relativistic collisionless pair shock. In particular, we provide a theoretical estimate of their scattering length lscatt(p) in the self-generated electromagnetic turbulence, as well as an estimate of their distribution function. We obtain lscatt(p)≈γpεB-1(p/γ∞mc)2c/ωp, with p the particle momentum in the rest frame of the shock front, εB the strength parameter of the microturbulence, γp the Lorentz factor of the background plasma relative to the shock front, and γ∞ its asymptotic value outside the precursor. We compare this scattering length to large-scale PIC simulations and find good agreement for the various dependencies.