ASTRA Proc., 1, 65-71, 2014
© Author(s) 2014. This work is distributed under
the Creative Commons Attribution 3.0 License.
31 Oct 2014
TeV Cosmic Ray Anisotropy and the Heliospheric Magnetic Field
P. Desiati1,2 and A. Lazarian2 1Wisconsin IceCube Particle Astrophysics Center (WIPAC), University of Wisconsin, Madison, WI 53703, USA
2Department of Astronomy, University of Wisconsin, Madison, WI 53706, USA
Abstract. Cosmic rays are observed to possess a small non uniform distribution in arrival direction. Such anisotropy appears to have a roughly consistent topology between tens of GeV and hundreds of TeV, with a smooth energy dependency on phase and amplitude. Above a few hundreds of TeV a sudden change in the topology of the anisotropy is observed. The distribution of cosmic ray sources in the Milky Way is expected to inject anisotropy on the cosmic ray flux. The nearest and most recent sources, in particular, are expected to contribute more significantly than others. Moreover the interstellar medium is expected to have different characteristics throughout the Galaxy, with different turbulent properties and injection scales. Propagation effects in the interstellar magnetic field can shape the cosmic ray particle distribution as well. In particular, in the 1–10 TeV energy range, they have a gyroradius comparable to the size of the Heliosphere, assuming a typical interstellar magnetic field strength of 3 μG. Therefore they are expected to be strongly affected by the Heliosphere in a manner ordered by the direction of the local interstellar magnetic field and of the heliotail. In this paper we discuss on the possibility that TeV cosmic rays arrival distribution might be significantly redistributed as they propagate through the Heliosphere.

Citation: Desiati, P. and Lazarian, A.: TeV Cosmic Ray Anisotropy and the Heliospheric Magnetic Field, ASTRA Proc., 1, 65-71,, 2014.
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