02 Oct 2015
02 Oct 2015
Cosmic ray transport and anisotropies to high energies
P. L. Biermann1,2,3,4, L. I. Caramete5, A. Meli6, B. N. Nath7, E.-S. Seo8, V. de Souza9, and J. Becker Tjus10
P. L. Biermann et al.
P. L. Biermann1,2,3,4, L. I. Caramete5, A. Meli6, B. N. Nath7, E.-S. Seo8, V. de Souza9, and J. Becker Tjus10
- 1MPI for Radioastronomy, Bonn, Germany
- 2Department of Physics, Karlsruhe Institute for Technology KIT, Karlsruhe, Germany
- 3Department of Physics & Astronomy, University of Alabama, Tuscaloosa, AL, USA
- 4Department of Physics & Astronomy, University Bonn, Bonn, Germany
- 5Institute for Space Sciences, Bucharest, Romania
- 6Department of Physics and Astronomy, University of Gent, Gent, Belgium
- 7Raman Research Institute, Bangalore, India
- 8Department of Physics, University of Maryland, College Park, MD, USA
- 9University de São Paulo, Inst. de Física de São Carlos, São Carlos, Brazil
- 10Department of Physics, University Bochum, Bochum, Germany
- 1MPI for Radioastronomy, Bonn, Germany
- 2Department of Physics, Karlsruhe Institute for Technology KIT, Karlsruhe, Germany
- 3Department of Physics & Astronomy, University of Alabama, Tuscaloosa, AL, USA
- 4Department of Physics & Astronomy, University Bonn, Bonn, Germany
- 5Institute for Space Sciences, Bucharest, Romania
- 6Department of Physics and Astronomy, University of Gent, Gent, Belgium
- 7Raman Research Institute, Bangalore, India
- 8Department of Physics, University of Maryland, College Park, MD, USA
- 9University de São Paulo, Inst. de Física de São Carlos, São Carlos, Brazil
- 10Department of Physics, University Bochum, Bochum, Germany
Correspondence: P. L. Biermann (plbiermann@mpifr-bonn.mpg.de)
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Received: 09 May 2015 – Revised: 14 Aug 2015 – Accepted: 09 Sep 2015 – Published: 02 Oct 2015
A model is introduced, in which the irregularity spectrum of the Galactic magnetic field beyond the dissipation length scale is first a Kolmogorov spectrum k-5/3 at small scales λ = 2 π/k with k the wave-number, then a saturation spectrum k-1, and finally a shock-dominated spectrum k-2 mostly in the halo/wind outside the Cosmic Ray disk. In an isotropic approximation such a model is consistent with the Interstellar Medium (ISM) data. With this model we discuss the Galactic Cosmic Ray (GCR) spectrum, as well as the extragalactic Ultra High Energy Cosmic Rays (UHECRs), their chemical abundances and anisotropies. UHECRs may include a proton component from many radio galaxies integrated over vast distances, visible already below 3 EeV.
