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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High-redshift AGN emitting UHE protons up to 10^19 eV generate a 50 PeV cosmogenic neutrino bump consistent with IceCube data from their JWST-measured average properties without fine-tuning.
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.
Minimal UHECR flux models from the Telescope Array predict cosmogenic neutrino fluxes consistent with the KM3-230213A event at the 2σ level.
citing papers explorer
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Ultraheavy Ultrahigh-Energy Cosmic Rays
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.
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Ultrahigh-energy cosmogenic neutrino emissions in the high-redshift universe
High-redshift AGN emitting UHE protons up to 10^19 eV generate a 50 PeV cosmogenic neutrino bump consistent with IceCube data from their JWST-measured average properties without fine-tuning.
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The Sensitivity of PUEO to Cosmogenic Neutrinos and Exotic Physics Scenarios
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.
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Ultra-high energy event KM3-230213A as a cosmogenic neutrino in light of minimal UHECR flux models
Minimal UHECR flux models from the Telescope Array predict cosmogenic neutrino fluxes consistent with the KM3-230213A event at the 2σ level.