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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Nonthermal radiation of young supernova remnants: the case of rx j1713.7–3946
TL;DR: In this article, a new numerical code was designed for the detailed numerical treatment of nonlinear diffusive shock acceleration, which is used for the modeling of particle acceleration and radiation in young supernova remnants (SNRs).
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On the spectrum of high-energy cosmic rays produced by supernova remnants in the presence of strong cosmic-ray streaming instability and wave dissipation
V. S. Ptuskin,V. N. Zirakashvili +1 more
TL;DR: In this article, the authors show that the maximum energy of the accelerated particles strongly depends on the age of a SNR and that the average spectrum of cosmic rays injected in the interstellar medium in the course of the adiabatic SNR evolution (the Sedov stage) is approximately Q(p)p 2 ∝ p −2 at energies larger than 10−30 GeV/nucleon and with a maximum particle energy that is close to the position of the knee in the cosmic-ray spectrum observed at ∼4 × 10 15 eV.
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Simulations of ion acceleration at non-relativistic shocks. II. Magnetic field amplification
TL;DR: In this article, the authors used large hybrid simulations to study ion acceleration and generation of magnetic turbulence due to the streaming of particles that are self-consistently accelerated at non-relativistic shocks.
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Toward understanding the cosmic-ray acceleration at young supernova remnants interacting with interstellar clouds: possible applications to rx j1713.7–3946
TL;DR: In this paper, the authors used three-dimensional magnetohydrodynamic simulations to investigate general properties of a blast wave shock interacting with interstellar clouds and found that the energy density of the amplified magnetic field locally grows comparable to the thermal energy density, particularly at the transition layers between clouds and their diffuse surrounding.
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Long-Term Evolution of Magnetic Turbulence in Relativistic Collisionless Shocks: Electron-Positron Plasmas
TL;DR: In this article, the authors study the long term evolution of magnetic fields generated by an initially unmagnetized collisionless relativistic e+e− shock and show that magnetic fields start with magnetic energy density ~ 0.1-0.2, but rapid downstream decay drives the fields to much smaller values, below ~10−3 of equipartition after ~103 skin depths.