Diffusion and drift of cosmic rays in highly turbulent magnetic fields

Abstract

We determine numerically the parallel, perpendicular, and antisymmetric diffusion coefficients for charged particles propagating in highly turbulent magnetic fields, by means of extensive Monte Carlo simulations. We propose simple expressions, given in terms of a small set of fitting parameters, to account for the diffusion coefficients as functions of magnetic rigidity and turbulence level, and corresponding to different kinds of turbulence spectra. The results obtained satisfy scaling relations, which make them useful for describing the cosmic ray origin and transport in a variety of different astrophysical environments.

17 pages, 7 figures

References in corpus (5)

• Transport of Cosmic Rays in Chaotic Magnetic Fields
• Lensing of ultra-high energy cosmic rays in turbulent magnetic fields
• Cosmic ray spectrum and anisotropies from the knee to the second knee
• Turbulent diffusion and drift in galactic magnetic fields and the explanation of the knee in the cosmic ray spectrum
• Cosmic ray drift, the second knee and galactic anisotropies

Cited by in corpus (41)

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• Dots, clumps and filaments: the intermittent images of synchrotron emission in random magnetic fields of young supernova remnants
• The optical depth of the Universe to ultrahigh energy cosmic ray scattering in the magnetized large scale structure
• Global diffusion of cosmic rays
• Inhomogeneous extragalactic magnetic fields and the second knee in the cosmic ray spectrum
• Cosmic Rays in Intermittent Magnetic Fields
• Magnetic diffusion effects on the Ultra-High Energy Cosmic Ray spectrum and composition
• Turbulence-Level Dependence of Cosmic-Ray Parallel Diffusion
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• High rigidity Forbush decreases: due to CMEs or shocks?
• Regimes of cosmic-ray diffusion in Galactic turbulence
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• Postshock turbulence and diffusive shock acceleration in young supernova remnants
• Cosmic ray acceleration at perpendicular shocks in supernova remnants
• Modulation of Galactic Cosmic Rays in the Inner Heliosphere over Solar Cycles
• Forbush decreases and turbulence levels at CME fronts
• Relative distribution of cosmic rays and magnetic fields
• Particle Transport in intense small scale magnetic turbulence with a mean field
• Modulation of Galactic Cosmic Rays in the Inner Heliosphere, Comparing with PAMELA Measurements
• Diffuse Neutrino and Gamma-ray Emissions of the Galaxy above the TeV
• On numerical turbulence generation for test-particle simulations
• How are Forbush decreases related to interplanetary magnetic field enhancements ?
• GeV-TeV Cosmic Ray Leptons in the Solar System from the Bow Shock Wind Nebula of the Nearest Millisecond Pulsar J0437-4715
• Cosmic Ray propagation in sub-Alfvenic magnetohydrodynamic turbulence
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• Relative contribution of the magnetic field barrier and solar wind speed in ICME-associated Forbush decreases
• Understanding Forbush decrease drivers based on shock-only and CME-only models using global signature of February 14, 1978 event
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• Anisotropic cosmic-ray diffusion in isotropic Kolmogorov turbulence
• Detectable neutrino fluxes due to enhanced cosmic ray densities in the Galactic Center region
• Turbulence and Anomalous Resistivity inside Near-Earth Magnetic Clouds
• Acceleration of cosmic rays in presence of magnetohydrodynamic fluctuations at small scales
• Interplay of large-scale drift and turbulence in the heliospheric propagation of solar energetic particles
• Hybrid viscosity and the magnetoviscous instability in hot, collisionless accretion disks
• Transport of charged particles propagating in turbulent magnetic fields as a red-noise process
• Velocity decorrelation functions of high-energy cosmic rays propagating in magnetic fields