Cosmic ray transport and anisotropies

Abstract

We show that the large-scale cosmic ray anisotropy at ~10 TeV can be explained by a modified Compton-Getting effect in the magnetized flow field of old supernova remnants. This approach suggests an optimum energy scale for detecting the anisotropy. Two key assumptions are that propagation is based on turbulence following a Kolmogorov law and that cosmic ray interactions are dominated by transport through stellar winds of the exploding stars. A prediction is that the amplitude is smaller at lower energies due to incomplete sampling of the velocity field and also smaller at larger energies due to smearing.

6 pages, 1 figure

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Cited by in corpus (10)

• Anisotropy in Cosmic-Ray Arrival Directions in the Southern Hemisphere with Six Years of Data from the IceCube Detector
• Origin of Small-Scale Anisotropies in Galactic Cosmic Rays
• Anomalous Anisotropies of Cosmic Rays from Turbulent Magnetic Fields
• Neutrinos and Cosmic Rays Observed by IceCube
• Cosmic Ray Small Scale Anisotropies and Local Turbulent Magnetic Fields
• Magnetic fields and cosmic ray anisotropies at TeV energies
• A New Maximum-Likelihood Technique for Reconstructing Cosmic-Ray Anisotropy at All Angular Scales
• Observation of TeV-PeV cosmic ray anisotropy with IceCube, IceTop and AMANDA
• Constraints on supermassive black hole spins from observations of active galaxy jets
• Cosmic Ray transport in mixed magnetic fields and their role on the observed anisotropies