Fine structure in the gamma-ray sky and the origin of UHECR

Simple item page
dc.creatorErlykin, A. D.
dc.creatorWolfendale, A. W.
dc.date2006-12-07
dc.date.accessioned2026-07-07T11:00:24Z
dc.date.available2026-07-07T11:00:24Z
dc.descriptionThe EGRET results for gamma ray intensities in and near the Galactic Plane have been analysed in some detail. Attention has been concentrated on energies above 1 GeV and the individual intensities in a $4^{\circ}$ longitude bin have been determined and compared with the large scale mean found from a nine-degree polynomial fit. Comparison has been made of the observed standard deviation for the ratio of these intensities with that expected from variants of our model. The basic model adopts cosmic ray origin from supernova remnants, the particles then diffusing through the Galaxy with our usual `anomalous diffusion'. The variants involve the clustering of SN, a frequency distribution for supernova explosion energies, and 'normal', rather than 'anomalous' diffusion. It is found that for supernovae of unique energy, and our usual anomalous diffusion, clustering is necessary, particularly in the Inner Galaxy. An alternative, and preferred, situation is to adopt the model with a frequency distribution of supernova energies. The results for the Outer Galaxy are such that no clustering is required. If their explosion energies are distributed then supernovae can be the origin of UHECR.
dc.description8 pages, 5 figures and 1 table, to appear in the proceedings of the CRIS2006 symposium, Catania, Italy, May-June 2006
dc.identifierhttps://arxiv.org/abs/astro-ph/0612181
dc.identifierhttp://arxiv.org/abs/astro-ph/0612181
dc.identifierNucl.Phys.Proc.Suppl.165:137-144,2007
dc.identifierdoi:10.1016/j.nuclphysbps.2006.11.020
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/187670
dc.subjectAstrophysics
dc.titleFine structure in the gamma-ray sky and the origin of UHECR
dc.typetext

Files

Collections

arXiv