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Enhancing the relative Fe-to-proton abundance in ultra-high-energy cosmic rays
Blaksley C., Parizot E.
Astroparticle Physics 35 (2012) 342-345 - http://hal.in2p3.fr/in2p3-00676839
Planète et Univers/Astrophysique/Phénomènes cosmiques de haute energie
Physique/Astrophysique/Phénomènes cosmiques de haute energie
Enhancing the relative Fe-to-proton abundance in ultra-high-energy cosmic rays
C. Blaksley1, E. Parizot1
1 :  APC - UMR 7164 - AstroParticule et Cosmologie
CNRS : UMR7164 – IN2P3 – Observatoire de Paris – Université Paris VII - Paris Diderot – CEA : DSM/IRFU
APC - UMR 7164, Université Paris Diderot, 10 rue Alice Domon et Léonie Duquet, case postale 7020, F-75205 Paris Cedex 13
We study a generic class of models for ultra-high energy cosmic ray (UHECR) phenomenology, in which the sources accelerate protons and nuclei with a power-law spectrum having the same index, but with different values for the maximum proton energies, distributed according to a power-law. We show that, for energies sufficiently lower than the maximum proton energy, such models are equivalent to single-type source models, with a larger effective power law index and a heavier composition at the source. We calculate the resulting enhancement of the abundance of nuclei, and find typical values of a factor 2-10 for Fe nuclei. At the highest energies, the heavy nuclei enhancement ratios become larger, and the granularity of the sources must also be taken into account. We conclude that the effect of a distribution of maximum energies among sources must be considered in order to understand both the energy spectrum and the composition of UHECRs, as measured on Earth.

Articles dans des revues avec comité de lecture
Astroparticle Physics (Astropart. Phys.)
Publisher Elsevier
ISSN 0927-6505 

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