| Issue |
EPJ Web Conf.
Volume 210, 2019
Ultra High Energy Cosmic Rays 2018 (UHECR 2018)
|
|
|---|---|---|
| Article Number | 04002 | |
| Number of page(s) | 6 | |
| Section | Phenomenology | |
| DOI | https://doi.org/10.1051/epjconf/201921004002 | |
| Published online | 17 May 2019 | |
https://doi.org/10.1051/epjconf/201921004002
Cosmic ray acceleration to ultrahigh energy in radio galaxies
1
University of Oxford, Astrophysics, Keble Road, Oxford, OX1 3RH, UK
2
University of Oxford, Clarendon Laboratory, Parks Road, Oxford OX1 3PU, UK
3
Astronomical Institute, Academy of Sciences of the Czech Republic, Boční II1401, CZ-141 00 Prague, Czech Republic
4
ELI Beamlines, Institute of Physics, Czech Academy of Sciences, 25241 Dolní Břežany, Czech Republic
* e-mail: james.matthews@physics.ox.ac.uk
Published online: 17 May 2019
The origin of ultrahigh energy cosmic rays (UHECRs) is an open question. In this proceeding, we first review the general physical requirements that a source must meet for acceleration to 10-100 EeV, including the consideration that the shock is not highly relativistic. We show that shocks in the backflows of radio galaxies can meet these requirements. We discuss a model in which giant-lobed radio galaxies such as Centaurus A and Fornax A act as slowly-leaking UHECR reservoirs, with the UHECRs being accelerated during a more powerful past episode. We also show that Centaurus A, Fornax A and other radio galaxies may explain the observed anisotropies in data from the Pierre Auger Observatory, before examining some of the difficulties in associating UHECR anisotropies with astrophysical sources.
© The Authors, published by EDP Sciences, 2019
This is an open access article distributed under the terms of the Creative Commons Attribution License 4.0 (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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