MHD Turbulence and Cosmic Ray Reacceleration in Galaxy Clusters

Abstract

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 1/4 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 haloes and the unobserved diffuse gamma-ray emission from these clusters.

References in corpus (20)

• Wilkinson Microwave Anisotropy Probe (WMAP) Three Year Results: Implications for Cosmology
• Heating Hot Atmospheres with Active Galactic Nuclei
• Clusters of galaxies : observational properties of the diffuse radio emission
• Testing X-ray Measurements of Galaxy Clusters with Cosmological Simulations
• Particle Acceleration on Megaparsec Scales in a Merging Galaxy Cluster
• Compressible Turbulence in Galaxy Clusters: Physics and Stochastic Particle Re-acceleration
• On the connection between giant radio halos and cluster mergers
• A low-frequency radio halo associated with a cluster of galaxies
• Cluster Magnetic Fields from Galactic Outflows
• The intracluster magnetic field power spectrum in Abell 2255
• Rise and Fall of Radio Halos in Simulated Merging Galaxy Clusters
• New scaling relations in cluster radio halos and the re-acceleration model
• Diffuse radio emission from clusters in the MareNostrum Universe simulation
• Hydrodynamical adaptive mesh refinement simulations of turbulent flows - II. Cosmological simulations of galaxy clusters
• Modeling the Large Scale Structures of Astrophysical Jets in the Magnetically Dominated Limit
• Probing the origin of giant radio halos through radio and gamma-ray data : the case of the Coma cluster
• Cosmic Ray Scattering in Compressible Turbulence
• First LOFAR observations at very low frequencies of cluster-scale non-thermal emission: the case of Abell 2256
• Comparisons of Cosmological MHD Galaxy Cluster Simulations to Radio Observations
• Formation of X-Ray Cavities by the Magnetically Dominated Jet-Lobe System in a Galaxy Cluster

Cited by in corpus (18)

• Cosmic rays in galaxy clusters and their non-thermal emission
• Stochastic reacceleration of relativistic electrons by turbulent reconnection: a mechanism for cluster-scale radio emission ?
• Turbulence and Particle Acceleration in Giant Radio Haloes: the Origin of Seed Electrons
• Relativistic protons in the Coma galaxy cluster: first gamma-ray constraints ever on turbulent reacceleration
• The Matryoshka Run (II): Time Dependent Turbulence Statistics, Stochastic Particle Acceleration and Microphysics Impact in a Massive Galaxy Cluster
• MHD Turbulence
• Turbulent Amplification and Structure of the Intracluster Magnetic Field
• The Planck clusters in the LOFAR sky: IV: LoTSS-DR2: statistics of radio halos and re-acceleration models
• An Efficient Fokker-Planck Solver and its Application to Stochastic Particle Acceleration in Galaxy Clusters
• The LOFAR and JVLA view of the distant steep spectrum radio halo in MACS J1149.5+2223
• Cosmic Magnetism in Centimeter and Meter Wavelength Radio Astronomy
• MHD Turbulence, Turbulent Dynamo and Applications
• Deep low-frequency radio observations of Abell 2256 II: The ultra-steep spectrum radio halo
• A three-component giant radio halo: the puzzling case of the galaxy cluster Abell 2142
• Is the Sunyaev-Zeldovich effect responsible for the observed steepening in the spectrum of the Coma radio halo ?
• A giant radio halo in a low-mass SZ-selected galaxy cluster: ACT-CL J0256.5+0006
• The Flow Around a Cosmic String, Part I: Hydrodynamic Solution
• Statistical signatures of interstellar turbulence in dust polarization maps