2007/06/25 by Hajime Takami, Katsuhiko Sato, Takami, Hajime +2
Physics and Astronomy · #Astrophysics (astro-ph) #Astrophysics and Cosmic Phenomena #Dark Matter and Cosmic Phenomena #FOS: Physical sciences #Neutrino Physics Research #astro-ph
paper · pdf · doi:10.48550/arxiv.0706.3666
Contribution to the 30th International Cosmic Ray Conference, Merida Mexico, July 2007, a corrected version; 4 pages, 3 figures
arxiv created 2007/06/25 · openalex publication_date 2007/06/25 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We simulate the arrival distribution of ultra-high-energy (UHE) protons by following their propagation processes in several strengths of a structured extragalactic magnetic field (EGMF). Comparing our result to observational one by Akeno Giant Air Shower Array, we constrain the number density of UHE cosmic ray sources with the small-scale anisotropy. As a result, the source number density is ∼ 10-5 \rm Mpc-3 with uncertainty of about an order of magnitude due to the small number of observed events. This hardly depends on our structured EGMF strength. We also investigate future prospects for this approarch. The near future observations, such as Pierre Auger Observatory, can distinguish 10-6 \rm Mpc-3 accurately from the more source densities. Number of events to discriminate between 10-4 and 10-5 \rm Mpc-3 is dependent on the EGMF strength.