2013/01/30 by Andrey Beresnyak, Hao Xu, Hui Li +1
Engineering · Physics and Astronomy · #Astronomy and Astrophysical Research #Cluster (spacecraft) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Magnetohydrodynamic drive #Magnetohydrodynamic turbulence #Magnetohydrodynamics #Proton #Space Technology and Applications #Turbulence #astro-ph.CO #astro-ph.GA
paper · pdf · doi:10.1088/0004-637x/771/2/131
arxiv created 2013/01/30 · openalex publication_date 2013/06/25 · arxiv updated 2015/06/12 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Cosmological MHD simulations of galaxy cluster formation show a significant amplification of seed magnetic fields. We developed a novel method to decompose cluster magnetized turbulence into modes and showed that the fraction of the fast mode is fairly large, around one-fourth in terms of energy. This is larger than that was estimated before, which implies that cluster turbulence interacts with cosmic rays rather efficiently. We propose a framework to deal with electron and proton reacceleration in galaxy clusters that includes feedback on turbulence. In particular, we establish a new upper limit on proton and electron fluxes based on turbulence intensity. These findings, along with detailed modeling of reacceleration, will help to reconcile the observed giant radio halos and the unobserved diffuse γ-ray emission from these clusters.