The acceleration of cosmic rays in shock fronts – I
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This article is published in Monthly Notices of the Royal Astronomical Society.The article was published on 1978-02-01 and is currently open access. It has received 2613 citations till now. The article focuses on the topics: Shock waves in astrophysics & Fermi acceleration.read more
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Cosmic ray current driven turbulence in shocks with efficient particle acceleration: the oblique, long-wavelength mode instability
TL;DR: In this paper, a multiscale, quasi-linear analysis of the response of the magnetized cosmic rays (CRs) current on magnetic field fluctuations is presented, and it is shown that the presence of turbulence with scales shorter than the CR gyroradius enhances the growth of modes with scales longer than the CRS, at least for particular polarizations.
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Resistive Magnetic Field Generation at Cosmic Dawn
TL;DR: In this article, it was shown that a magnetic field is robustly generated throughout intergalactic space at a rate of 10?17 to 10?16?G?Gyr?1, until the temperature of the inter-galactic medium is raised by cosmic reionization.
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Non-Thermal Electron Acceleration in Low Mach Number Collisionless Shocks. I. Particle Energy Spectra and Acceleration Mechanism
TL;DR: In this article, the authors used two-and three-dimensional particle-in-cell plasma simulations to study electron acceleration in low Mach number (M < 5) shocks and found that about 15 percent of the electrons can be efficiently accelerated, forming a non-thermal power-law tail in the energy spectrum with a slope of p~2.4.
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High-Energy Cosmic Rays from Gamma-Ray Burst Sources: A Stronger Case
TL;DR: In this article, the authors show that the constraints that UHECR sources must satisfy in order to allow proton acceleration to greater than 1020 eV are similar to those inferred for GRB sources from γ-ray observations.
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Ion Superdiffusion at the Solar Wind Termination Shock
Silvia Perri,Gaetano Zimbardo +1 more
TL;DR: In this paper, the authors investigate the propulsion of 0.54-3.5 MeV ions accelerated at the termination shock of the solar wind and find that transport is superdiffusive, with a mean square deviation growing like Δx 2 ∝ t α.