Anisotropic diffusion and the cosmic ray anisotropy

Abstract

We argue that the diffusion of cosmic rays in the Galactic magnetic field has to be strongly anisotropic. As a result, the number of CR sources contributing to the local CR flux is reduced by a factor $\sim 200$. The CR density is therefore less smooth, and the contribution of individual sources to the CR dipole anisotropy becomes more prominent. In the case of anisotropic diffusion, the observed plateau in the CR dipole anisotropy around 2-20 TeV can be explained by a 2-3 Myr old CR source which dominates the local CR flux in this energy range.

arXiv comment6 pages, 5 eps figures; invited talk at the 26th Extended European Cosmic Ray Symposium, 2018

References in corpus (9)

• The Galactic Magnetic Field
• Cosmic-Ray Nuclei, Antiprotons and Gamma-rays in the Galaxy: a New Diffusion Model
• Bayesian analysis of cosmic-ray propagation: evidence against homogeneous diffusion
• Signatures of a two million year old supernova in the spectra of cosmic ray protons, antiprotons and positrons
• Deciphering the Dipole Anisotropy of Galactic Cosmic Rays
• Origin of Small-Scale Anisotropies in Galactic Cosmic Rays
• Spectrum and Anisotropy of Cosmic Rays at TeV-PeV-energies and Contribution of Nearby Sources
• Reconciling cosmic ray diffusion with Galactic magnetic field models
• Solution to the cosmic ray anisotropy problem

Cited by in corpus (2)

• Possible bump structure of cosmic ray electrons unveiled by AMS-02 data and its common origin along with the nuclei and positron
• Study of Galactic interactions and propagation properties of ultrahigh energy cosmic rays using the precision spectrum from the Pierre Auger Observatory