Heliospheric Boundary and the TeV Cosmic Ray Anisotropy

Cosmic Ray Anisotropy Workshop 2013

Desiati, Paolo^1,2 ; Lazarian, Alex^2

Wisconsin IceCube Particle Astrophysics Center (WIPAC), University of Wisconsin, Madison, WI 53703, United States^1

Department of Astronomy, University of Wisconsin, Madison, WI 53706, United States^2

关键词: Arrival direction;    Cosmic ray anisotropy;    Cosmic-ray particles;    Energy dependency;    Heliospheric magnetic fields;    Interstellar magnetic fields;    Non-uniform distribution;    Resonant scattering;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/531/1/012011/pdf
DOI  :  10.1088/1742-6596/531/1/012011

来源: IOP

【 摘 要 】

Observations over the last few decades have shown that cosmic rays have a small non uniform distribution in arrival direction. Such anisotropy appears to have a roughly consistent topology between 10's GeV and 100's TeV, with a smooth energy dependency on phase and amplitude. However, above a few 100's TeV a sudden change in the topology of the anisotropy is observed. The cosmic ray arrival directions are expected to depend on the distribution of their sources in the Milky Way, as well as on effects arising from propagation in the inhomogeneous and turbulent interstellar magnetic field. In particular, in the 1-10 TeV energy range, the gyroradius of cosmic ray particles, much smaller that the injection scale of interstellar magnetic field turbulence, is comparable to the size of the heliosphere. Resonant scattering processes of cosmic ray particles propagating through the heliosphere may be able to induce a redistribution of the small anisotropic component of their flux. In this paper we discuss on the processes that occurs to TeV cosmic rays in the heliosphere and on the possibility to probe the heliospheric magnetic fields on large scale by studying the arrival distribution of cosmos rays.