G. Giacinti, M. Kachelriess, D. V. Semikoz, G. Sigl
Published 2011-04-06, updated 2011-09-05Version 2
In this work we study how the turbulent component of the Galactic magnetic field (GMF) affects the propagation of ultrahigh energy heavy nuclei. We investigate first how the images of individual sources and of the supergalactic plane depend on the properties of the turbulent GMF. Then we present a quantitative study of the impact of the turbulent field on (de-) magnification of source fluxes, due to magnetic lensing effects. We also show that it is impossible to explain the Pierre Auger data assuming that all ultrahigh energy nuclei are coming from Cen A, even in the most favorable case of a strong, extended turbulent field in the Galactic halo.
Comments: 10 pages (2 columns), 8 figures. Published in Astroparticle Physics
Journal: Astropart. Phys. 35, 192-200 (2011)
Propagation of ultrahigh energy nuclei in clusters of galaxies: resulting composition and secondary emissions
The fate of ultrahigh energy nuclei in the immediate environment of young fast-rotating pulsars
Explaining the Spectra of Cosmic Ray Groups above the Knee by Escape from the Galaxy
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