The propagation of UHECRs is affected by the intergalactic magnetic field that was produced during the course of the large scale structure formation of the universe. Adopting a novel model based on turbulent dynamo, the strength of the intergalactic magnetic field is estimated from local dynamic properties of the gas flows in hydrodynamic simulations of a concordance LCDM universe. The direction of the magnetic field is taken as that of the passively evolved field. With the model magnetic field, the deflection angle and time delay are calculated for protons with E > 10^19 eV propagating through the large scale structure of the universe, as well as the energy loss due to interactions with cosmic background radiation. Implications of this study on the origin of UHECRs are discussed.

This work is supported by KOSEF through the Astrophysical Research Center for the Structure and Evolution of Cosmos (ARCSEC).

Proceedings of the 30th International Cosmic Ray Conference; Rogelio Caballero, Juan Carlos D'Olivo, Gustavo Medina-Tanco, Lukas Nellen, Federico A. Sánchez, José F. Valdés-Galicia (eds.); Universidad Nacional Autónoma de México, Mexico City, Mexico, 2008; Vol. 2 (OG part 1), pages 175-178