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The large scale structure of the Galactic magnetic field and High Energy Cosmic Ray anisotropy

Jaime Alvarez-Muñiz·Todor Stanev
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Abstract

The magnetic field in our Galaxy is not well known and is difficult to measure. A spiral regular field in the disk between the Galactic arms is favored by observations, however it is still controversial if the field reverses from arm to arm. The parity of the field across the Galactic plane is also not well established. In this letter we demonstrate that cosmic ray protons in the energy range 10^18 to 10^19 eV, if accelerated near the center of the Galaxy, can probe the large scale structure of the Galactic Magnetic Field. In particular if the field is of even parity, and the spiral field reverses direction from arm to arm, i.e. if it is bi-symmetric (BSS), ultra high energy protons will predominantly come from the Southern Galactic hemisphere, and predominantly from the Northern Galactic hemisphere if the field is of even parity and axi-symmetric (ASS). There is no sensitivity to the BSS or ASS configurations if the field is of odd parity.

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Jaime Alvarez-Muñiz, Todor Stanev. 2005-07-12. The large scale structure of the Galactic magnetic field and High Energy Cosmic Ray anisotropy. https://doi.org/10.1088/1742-6596%2F47%2F1%2F016

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