Ultra-High Energy Cosmic Rays Detected by Auger and AGASA:Corrections for Galactic Magnetic Field Deflections, Source Populations, and Arguments for Multiple-ComponentsReport as inadecuate



 Ultra-High Energy Cosmic Rays Detected by Auger and AGASA:Corrections for Galactic Magnetic Field Deflections, Source Populations, and Arguments for Multiple-Components


Ultra-High Energy Cosmic Rays Detected by Auger and AGASA:Corrections for Galactic Magnetic Field Deflections, Source Populations, and Arguments for Multiple-Components - Download this document for free, or read online. Document in PDF available to download.

Download or read this book online for free in PDF: Ultra-High Energy Cosmic Rays Detected by Auger and AGASA:Corrections for Galactic Magnetic Field Deflections, Source Populations, and Arguments for Multiple-Components
The origin and composition of Ultra-High Energy Cosmic Ray Events UHECRs are under debate. Here we improve constraints on the source populations and compositions of UHECRs by accounting for UHECR deflections within existing Galactic magnetic field models GMFs. We used Monte Carlo simulations for UHECRs detected by the Pierre Auger Observatory and AGASA in order to determine their outside-the-Galaxy arrival directions, and compared these with Galactic and extragalactic sources. The simulations, which used UHECR compositions from protons to Iron and seven models of the ordered GMF, include uncertainties in the GMF and a turbulent magnetic field. The correlation between UHECRs and nearby extended radiogalaxies Nagar & Matulich 2008 remains valid, even strengthened, within several GMF models. Both the nearest radiogalaxy CenA, and the nearest radio-extended BL Lac, CGCG 413-019, are likely sources of multiple UHECRs. The correlation appears to be linked to the presence of the extended radio source rather than a tracer of an underlying population. It is possible, but unlikely, that all UHECRs originate in the nearby radiogalaxy CenA. For light UHECRs about a third of UHECRs can be -matched- to nearby galaxies with extended radio jets. The remaining UHECRs could also be explained as originating in extended radiogalaxies if one has at least one of: a large UHECR mean free path, a high cluster and-or intergalactic magnetic field, a heavy composition for two-thirds of the detected UHECRs. Several UHECRs have trajectories which pass close to Galactic magnetars and-or microquasars. If extended radiogalaxies are, or trace, UHECR sources, the most consistent models for the ordered GMF are the BS-S and BS-A models; the GMF models of Sun et al. 2008 are acceptable if a dipole component is added.



Author: Neil M. Nagar; Javier Matulich

Source: https://archive.org/







Related documents