The acceleration of cosmic rays in shock fronts – I
Reads0
Chats0
About:
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
Citations
More filters
Journal ArticleDOI
The Relation Between the Surface Brightness and the Diameter for Galactic Supernova Remnants
TL;DR: In this paper, a relation between the surface brightness and diameter (D) of Galactic C- and S-type supernova remnants (SNRs) has been constructed, and the relationship has been shown to have two slopes with a turning point at D=36.5 pc.
Journal ArticleDOI
Turbulence-induced magnetic fields in shock precursors
TL;DR: In this article, the authors explore the magnetic field amplification in different ISM conditions through 3D MHD numerical simulations and show that the inhomogeneities present in the interstellar medium (ISM) are the consequence of turbulence.
Book ChapterDOI
Particle Acceleration at Relativistic Shocks
TL;DR: In this article, the current status of Fermi acceleration theory at relativistic shocks is reviewed, and numerical calculations of the accelerated particle spectrum and the maximum energy attainable by this process are presented.
On the cosmological propagation of high energy particles in magnetic fields
TL;DR: In this article, the authors explored the connection between high energy particles and cosmic magnetic fields and explored the propagation of ultra-high energy cosmic rays (UHECRs) and very high energy gamma rays (VHEGRs) over cosmological distances.
Journal ArticleDOI
Bifurcation, Efficiency, and the Role of Injection in Shock Acceleration with the Bohm Diffusion
TL;DR: In this article, a manifold of all possible solutions in this parameter space was determined, and the authors showed that in contrast to the two-fluid model, three different solutions appeared together only if the injection rate? lies between two critical values,?1?2(M, p1), an efficient solution only occurs with a very high cosmic ray production rate.