Mapping Deflections of Extragalactic Ultra High Energy Cosmic Rays in Magnetohydrodynamic Simulations of the Local Universe

Details Mapping Deflections of Extragalactic Ultra High Energy Cosmic Rays in Magnetohydrodynamic Simulations of the Local Universe Mapping Deflections of Extragalactic Ultra High Energy Cosmic Rays in Magnetohydrodynamic Simulations of the Local Universe

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004nuphs.136..234d&link_type=abstract

Nuclear Physics B, Volume 136, p. 234-243.

Physics

Nuclear Physics

1

Scientific paper

We modeled the Extra Galactic Magnetic Fields in the nearby universe under the assumption that they are the outcome of a MHD amplification process which started from a magnetic seed generated at high redshift. These simulations successfully reproduce Faraday rotation measurements in galaxy clusters and provide new clues on the intensity and geometrical structure of magnetic fields in low density regions like filaments, sheets and voids. The initial conditions for the dark matter density fluctuations are constrained in such way that they reflect the observed density field within a sphere of a 110 Mpc radius around the Milky Way. Therefore, since the DM determines the dynamics of the entire system, the simulation should provide a reasonable description of the actual magnetic field large scale structure. We construct associated maps of deflections of protons under the action of the Lorentz force at energy E = 4 × 1019 eV and E = 1020 eV. Since in both cases we found deflection smaller than few degrees over most of sky area, we conclude that charge particle astronomy should be possible. At the end of this contribution we comment on possible reasons for the discrepant results presented by G. Sigl during this conference.

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