Simulations show that drift dominance over diffusion can create a knee at PeV energies if parallel diffusion becomes energy-independent above 1 TeV, though some setups fail to match observed grammage.
Wave damping by MHD turbulence and its effect upon cosmic ray propagation in the ISM
2 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
Cosmic rays scatter off magnetic irregularities (Alfven waves) with which they are resonant, that is waves of wavelength comparable to their gyroradii. These waves may be generated either by the cosmic rays themselves, if they stream faster than the Alfven speed, or by sources of MHD turbulence. Waves excited by streaming cosmic rays are ideally shaped for scattering, whereas the scattering efficiency of MHD turbulence is severely diminished by its anisotropy. We show that MHD turbulence has an indirect effect on cosmic ray propagation by acting as a damping mechanism for cosmic ray generated waves. The hot (``coronal'') phase of the interstellar medium is the best candidate location for cosmic ray confinement by scattering from self-generated waves. We relate the streaming velocity of cosmic rays to the rate of turbulent dissipation in this medium, for the case in which turbulent damping is the dominant damping mechanism. We conclude that cosmic rays with up to 10^2 GeV could not stream much faster than the Alfven speed, but that 10^6 GeV cosmic rays would stream unimpeded by self-generated waves unless the coronal gas were remarkably turbulence-free.
fields
astro-ph.HE 2years
2026 2verdicts
UNVERDICTED 2representative citing papers
SKA will enable spatially resolved radio studies of pulsar wind nebulae to probe particle acceleration and propagation in ultra-relativistic outflows.
citing papers explorer
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Transition from Diffusion to Drift-Dominated Cosmic Ray Transport and the Origin of the Knee
Simulations show that drift dominance over diffusion can create a knee at PeV energies if parallel diffusion becomes energy-independent above 1 TeV, though some setups fail to match observed grammage.
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Understanding Pulsar Wind Nebulae with the SKA
SKA will enable spatially resolved radio studies of pulsar wind nebulae to probe particle acceleration and propagation in ultra-relativistic outflows.