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Acceleration and radiation of ultra-high energy protons in galaxy clusters
Vannoni G., Aharonian F.A., Gabici S., Kelner S.R., Prosekin A.
Astronomy and Astrophysics 536 (2011) A56 - http://hal.in2p3.fr/in2p3-00730712
Planète et Univers/Astrophysique/Phénomènes cosmiques de haute energie
Physique/Astrophysique/Phénomènes cosmiques de haute energie
Acceleration and radiation of ultra-high energy protons in galaxy clusters
G. Vannoni1, F. A. Aharonian, S. Gabici2, S. R. Kelner, A. Prosekin
1 :  SPP - Service de Physique des Particules
http://www-dapnia.cea.fr/Spp/
CEA : DSM/IRFU
France
2 :  APC - UMR 7164 - AstroParticule et Cosmologie
http://www.apc.univ-paris7.fr/
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
France
APC - AHE
Context. Clusters of galaxies are believed to be capable of accelerating protons at accretion shocks to energies exceeding 1018 eV. At these energies, the losses caused by interactions of cosmic rays with photons of the cosmic microwave background radiation (CMBR) begin to have an effect and determine the maximum energy of protons and the shape of the energy spectrum in the cutoff region. Aims: The aim of this work is to study both the formation of the energy spectrum of accelerated protons at accretion shocks of galaxy clusters and the characteristics of their broad band emission. Methods: The proton energy distribution is calculated self-consistently via a time-dependent numerical treatment of the shock acceleration process, which takes the proton energy losses due to interactions with the CMBR into account. We calculate the energy distribution of accelerated protons, as well as the flux of broad-band emission produced by secondary electrons and positrons via synchrotron and inverse Compton scattering processes. Results: We find that the downstream and upstream regions contribute almost at the same level to the emission. For the typical parameters characterising galaxy clusters, the synchrotron and IC peaks in the spectral energy distributions appear at comparable flux levels. Conclusions: For an efficient acceleration, the expected emission components in the X-ray and gamma-ray bands are close to the detection threshold of current generation instruments, and will possibly be detected with the future generation of detectors. Remarkably, the acceleration of iron at these shocks can proceed up to a particle energy of ≈ 1020 eV, making clusters of galaxies possible contributors to the observed flux of ultra high energy cosmic rays.

Articles dans des revues avec comité de lecture
12/2011
Astronomy and Astrophysics (Astron. Astrophys.)
Publisher EDP Sciences
ISSN 0004-6361 (eISSN : 1432-0756)
536
A56

acceleration of particles – shock waves – radiation mechanisms: non-thermal – galaxies: clusters: general