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.
Alves Batista et al
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If Little Red Dots accelerate protons to ~10 EeV, their interactions with the high-redshift CMB produce a ~50 PeV cosmogenic neutrino bump consistent with IceCube.
PUEO will constrain the proton fraction of ultrahigh-energy cosmic rays under strong source evolution and set leading neutrino constraints on ultraheavy dark matter decays and some cosmic string models above 10^19 eV.
Simulations show that drift dominance over diffusion can create a knee at PeV energies if parallel diffusion becomes energy-independent above 1 TeV, though some setups fail to match observed grammage.
Minimal UHECR flux models from the Telescope Array predict cosmogenic neutrino fluxes consistent with the KM3-230213A event at the 2σ level.
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Ultrahigh-energy cosmogenic neutrino emissions in the high-redshift universe
If Little Red Dots accelerate protons to ~10 EeV, their interactions with the high-redshift CMB produce a ~50 PeV cosmogenic neutrino bump consistent with IceCube.