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| HAL : hal-00713422, version 1 |
| arXiv : 1104.1141 |
| DOI : 10.1016/j.astropartphys.2011.07.006 |
| Fiche détaillée |  Récupérer au format |
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| Astroparticle Physics 35 (2011) 192 |
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| Ultrahigh Energy Nuclei in the Turbulent Galactic Magnetic Field |
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| G. Giacinti1, 2M. Kachelriess3D.V. Semikoz1G. Sigl1, 2 |
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| (11/2011) |
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| 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. |
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| 1 : | APC - AstroParticule et Cosmologie |
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| 2 : | ITP - Institut für Theoretische Physik |
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| 3 : | NTNU - Institutt for fysikk, NTNU |
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| APC - THEORIE |
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| Domaine | : | Physique/Astrophysique/Phénomènes cosmiques de haute energie Planète et Univers/Astrophysique/Phénomènes cosmiques de haute energie |
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| Lien vers le texte intégral : |
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| http://fr.arXiv.org/abs/1104.1141 |
| hal-00713422, version 1 | |
| http://hal.archives-ouvertes.fr/hal-00713422 | |
| oai:hal.archives-ouvertes.fr:hal-00713422 | |
| Contributeur : Dmitri Semikoz | |
| Soumis le : Dimanche 1 Juillet 2012, 09:02:24 | |
| Dernière modification le : Dimanche 1 Juillet 2012, 23:22:14 | |
