Ultraheavy nuclei have longer energy loss lengths at ≲300 EeV than lighter nuclei, allowing them to explain UHECRs above 100 EeV from sources like collapsars and neutron star mergers while predicting distinct shower maxima.
Very-High-Energy Gamma-Ray Signal from Nuclear Photodisintegration as a Probe of Extragalactic Sources of Ultrahigh-Energy Nuclei
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abstract
It is crucial to identify the ultrahigh-energy cosmic-ray (UHECR) sources and probe their unknown properties. Recent results from the Pierre Auger Observatory favor a heavy nuclear composition for the UHECRs. Under the requirement that heavy nuclei survive in these sources, using gamma-ray bursts as an example, we predict a diagnostic gamma-ray signal, unique to nuclei - the emission of de-excitation gamma rays following photodisintegration. These gamma rays, boosted from MeV to TeV-PeV energies, may be detectable by gamma-ray telescopes such as VERITAS, HESS, and MAGIC, and especially the next-generation CTA and AGIS. They are a promising messenger to identify and study individual UHE nuclei accelerators.
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The cosmologically integrated neutrino emission from supermassive black hole coronae in Seyfert galaxies can account for the sub-PeV diffuse extragalactic neutrino flux observed by IceCube.
Monte Carlo simulations of nuclear cascades in NGC 1068 demonstrate that injected nuclear composition imprints on neutrino and gamma-ray spectra, supported by a re-analysis of archival COMPTEL observations.
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Nuclei in high-energy neutrino sources: A multimessenger study of in-source propagation
Monte Carlo simulations of nuclear cascades in NGC 1068 demonstrate that injected nuclear composition imprints on neutrino and gamma-ray spectra, supported by a re-analysis of archival COMPTEL observations.