COSMIC-RAY TRANSPORT AND ANISOTROPIES

2012/06/05 by P. L. Biermann, Peter L. Biermann, J. K. Becker +5
Earth and Planetary Sciences · Physics and Astronomy · #Amplitude #Anisotropy #Astrophysics and Cosmic Phenomena #COSMIC cancer database #Cosmic ray #Dark Matter and Cosmic Phenomena #Earth Systems and Cosmic Evolution #Field (mathematics) #Magnetic field #Supernova #Turbulence #astro-ph.HE

paper · pdf · doi:10.1088/0004-637x/768/2/124

6 pages, 1 figure

arxiv created 2012/06/05 · openalex publication_date 2013/04/22 · arxiv updated 2015/06/05 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06

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. Cosmic rays arrive isotropically to the flow field and are then carried along with the flow to produce a large-scale anisotropy in the arrival direction. 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 via cosmic-ray-excited magnetic irregularities through the stellar wind of an exploding star and its shock shell. 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.

Citations

• CENTAURUS A: THE EXTRAGALACTIC SOURCE OF COSMIC RAYS WITH ENERGIES ABOVE THE KNEE
• The Contribution of Different Supernova Populations to the Galactic Gamma‐Ray Background
• Rapid Variability and Annual Cycles in the Characteristic Timescale of the Scintillating Source PKS 1257−326
• THE ORIGIN OF COSMIC RAYS: EXPLOSIONS OF MASSIVE STARS WITH MAGNETIC WINDS AND THEIR SUPERNOVA MECHANISM
• The Structure of the Local Interstellar Medium. I. High‐Resolution Observations of Fe ii , Mg ii , and Ca ii toward Stars within 100 Parsecs
• Dynamics of the Interplanetary Gas and Magnetic Fields.
• Amplification of Galactic Magnetic Fields by the Cosmic-Ray-driven Dynamo
• THE WMAP HAZE FROM THE GALACTIC CENTER REGION DUE TO MASSIVE STAR EXPLOSIONS AND A REDUCED COSMIC RAY SCALE HEIGHT
• TRIGONOMETRIC PARALLAXES OF MASSIVE STAR-FORMING REGIONS. VI. GALACTIC STRUCTURE, FUNDAMENTAL PARAMETERS, AND NONCIRCULAR MOTIONS
• Radioactive 26Al from massive stars in the Galaxy
• An improved map of the Galactic Faraday sky
• COSMIC-RAY PROTON AND HELIUM SPECTRA FROM THE FIRST CREAM FLIGHT
• The Three-Phase Interstellar Medium Revisited