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.
Askar’yan,Excess Negative Charge of an Electron-Photon Shower and its Coherent Radio Emission,Zh
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abstract
The Pierre Auger Observatory, located on a vast, high plain in western Argentina, is the world's largest cosmic ray observatory. The objectives of the Observatory are to probe the origin and characteristics of cosmic rays above $10^{17}$ eV and to study the interactions of these, the most energetic particles observed in nature. The Auger design features an array of 1660 water-Cherenkov particle detector stations spread over 3000 km$^2$ overlooked by 24 air fluorescence telescopes. In addition, three high elevation fluorescence telescopes overlook a 23.5 km$^2$, 61-detector infilled array with 750 m spacing. The Observatory has been in successful operation since completion in 2008 and has recorded data from an exposure exceeding 40,000 km$^2$ sr yr. This paper describes the design and performance of the detectors, related subsystems and infrastructure that make up the Auger Observatory.
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A reconstruction algorithm using the radio emission maximum X_radio_max distinguishes deeply developing neutrino-induced air showers from cosmic rays, enhancing sensitivity above 1 EeV for inclined events.
Updated Xmax measurements reveal a transition to heavier cosmic-ray mass composition above 10^18.4 eV with decreasing elemental diversity.
Transformers trained on cosmic ray simulations learn physically plausible features in positional encodings for symmetric air showers and in attention mechanisms for galaxy-origin particles.
BL Lacs remain consistent with UHECR observations while FSRQs are disfavoured by anisotropy and source density mismatches after propagation modeling.
Minimal UHECR flux models from the Telescope Array predict cosmogenic neutrino fluxes consistent with the KM3-230213A event at the 2σ level.
With 2013-2023 exposure, the as-built ARA achieves world-leading UHE neutrino sensitivity above ~10^19 eV and predicts up to 13 trigger-level events under optimistic flux models, with secondaries contributing up to 30% of acceptance.
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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Downward ultra-high-energy neutrino detection in the air with radio antennas at ground-based observatories
A reconstruction algorithm using the radio emission maximum X_radio_max distinguishes deeply developing neutrino-induced air showers from cosmic rays, enhancing sensitivity above 1 EeV for inclined events.
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Depth of Maximum of Air-Shower Profiles above 10^17.7 eV Measured with the Fluorescence Detector of the Pierre Auger Observatory
Updated Xmax measurements reveal a transition to heavier cosmic-ray mass composition above 10^18.4 eV with decreasing elemental diversity.
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What exactly did the Transformer learn from our physics data?
Transformers trained on cosmic ray simulations learn physically plausible features in positional encodings for symmetric air showers and in attention mechanisms for galaxy-origin particles.
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Study of Flat Spectrum Radio Quasars and BL Lacertae Objects as Sources of Diffusive Ultra High-Energy Cosmic Rays
BL Lacs remain consistent with UHECR observations while FSRQs are disfavoured by anisotropy and source density mismatches after propagation modeling.
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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.
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Sensitivity of the As-Built Askaryan Radio Array to Ultra-High Energy Neutrinos
With 2013-2023 exposure, the as-built ARA achieves world-leading UHE neutrino sensitivity above ~10^19 eV and predicts up to 13 trigger-level events under optimistic flux models, with secondaries contributing up to 30% of acceptance.