MAGNETOHYDRODYNAMIC TURBULENCE AND COSMIC-RAY REACCELERATION IN GALAXY CLUSTERS

被引:23
作者
Beresnyak, Andrey [1 ,2 ]
Xu, Hao [1 ,3 ]
Li, Hui [1 ]
Schlickeiser, Reinhard [2 ]
机构
[1] Los Alamos Natl Lab, Los Alamos, NM 87545 USA
[2] Ruhr Univ Bochum, D-44780 Bochum, Germany
[3] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA
基金
美国国家科学基金会;
关键词
acceleration of particles; galaxies: clusters: intracluster medium; turbulence; INTERGALACTIC MAGNETIC-FIELD; DIFFUSE RADIO-EMISSION; COMA CLUSTER; COSMOLOGICAL SIMULATIONS; PARTICLE REACCELERATION; COMPRESSIBLE TURBULENCE; INTERSTELLAR TURBULENCE; NONTHERMAL EMISSION; FERMI OBSERVATIONS; SCALING RELATIONS;
D O I
10.1088/0004-637X/771/2/131
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 gamma-ray emission from these clusters.
引用
收藏
页数:8
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