Ion injection at perpendicular shocks requires 3D geometry to capture the porosity of downstream magnetic turbulence that lets particles return upstream and gain energy.
Cluster magnetic fields from large-scale-structure and galaxy-cluster shocks
2 Pith papers cite this work. Polarity classification is still indexing.
2
Pith papers citing it
abstract
The origin of the micro-Gauss magnetic fields in galaxy clusters is one of the outstanding problem of modern cosmology. We have performed three-dimensional particle-in-cell simulations of the nonrelativistic Weibel instability in an electron-proton plasma, in conditions typical of cosmological shocks. These simulations indicate that cluster fields could have been produced by shocks propagating through the intergalactic medium during the formation of large-scale structure or by shocks within the cluster. The strengths of the shock-generated fields range from tens of nano-Gauss in the intercluster medium to a few micro-Gauss inside galaxy clusters.
fields
astro-ph.HE 2verdicts
UNVERDICTED 2representative citing papers
A self-consistent multi-zone kinetic model reproduces SN 1006's spectrum and morphology, finding ~20% CR acceleration efficiency in quasi-parallel shocks, <1% in quasi-perpendicular shocks, and predominantly leptonic gamma-ray emission.
citing papers explorer
-
The role of three-dimensional effects on ion injection and acceleration in perpendicular shocks
Ion injection at perpendicular shocks requires 3D geometry to capture the porosity of downstream magnetic turbulence that lets particles return upstream and gain energy.
-
SN 1006: A Cosmic Laboratory for Investigating Shock Acceleration Physics
A self-consistent multi-zone kinetic model reproduces SN 1006's spectrum and morphology, finding ~20% CR acceleration efficiency in quasi-parallel shocks, <1% in quasi-perpendicular shocks, and predominantly leptonic gamma-ray emission.