| Article | |
| Title | High-energy cosmic-ray acceleration |
| Author(s) | Bustamante, M (Lima, Pont. U. Catolica) ; Carrillo Montoya, G (EPFL, Lausanne ; Wisconsin U., Madison) ; de Paula, W (Sao Paulo, Inst. Tech. Aeronautics) ; Duarte Chavez, J A (Colombia, U. Natl.) ; Gago, A M (Lima, Pont. U. Catolica) ; Hakobyan, H (Santa Maria U., Valparaiso) ; Jez, P (Bohr Inst.) ; Monroy Montañez, J A (Andes U., Bogota) ; Ortiz Velasquez, A (Mexico U., ICN) ; Padilla Cabal, F (InSTEC, La Habana, Cuba) ; Pino Rozas, M (Chile U., Catolica) ; Rodriguez Patarroyo, D J (Antonio Narino U.) ; Romeo, G L (Buenos Aires U.) ; Saldaña-Salazar , U J (UNAM, Mexico) ; Velasquez, M (Antioquia U.) ; von Steinkirch, M (Sao Paulo U.) |
| Publication | CERN, 2010 |
| In: | 2009 CERN - Latin-American School of High-Energy Physics, pp.533-540 |
| DOI | 10.5170/CERN-2010-001.533 |
| Abstract | We briefly review the basics of ultrahigh-energy cosmic-ray acceleration. The Hillas criterion is introduced as a geometrical criterion that must be fulfilled by potential acceleration sites, and energy losses are taken into account in order to obtain a more realistic scenario. The different available acceleration mechanisms are presented, with special emphasis on Fermi shock acceleration and its prediction of a power-law cosmic-ray energy spectrum. We conclude that first-order Fermi acceleration, though not entirely satisfactory, is the most promising mechanism for explaining the ultra-high-energy cosmic-ray flux. |
| Copyright/License | publication: © 2010-2024 CERN (License: CC-BY-3.0) |
Element opprettet 2010-03-19, sist endret 2022-08-10