2015/05/08 by Anabella Araudo, Anabella T. Araudo, Anthony R. Bell +5
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE) #Radio Astronomy Observations and Technology #Solar and Space Plasma Dynamics #astro-ph.HE
paper · pdf · doi:10.48550/arxiv.1505.02210
Accepted for publication in ApJ. 6 pages - 2 figures. Minor corrections
openalex publication_date 2015/05/08 · arxiv created 2015/06/07 · arxiv updated 2015/06/09 · openalex created_date 2022/09/18 · openalex updated_date 2026/07/28
We model the multi-wavelength emission in the southern hotspot of the radio quasar 4C74.26. The synchrotron radio emission is resolved near the shock with the MERLIN radio-interferometer, and the rapid decay of this emission behind the shock is interpreted as the decay of the amplified downstream magnetic field as expected for small scale turbulence. Electrons are accelerated to only 0.3 TeV, consistent with a diffusion coefficient many orders of magnitude greater than in the Bohm regime. If the same diffusion coefficient applies to the protons, their maximum energy is only ~100 TeV.