Astrophysical Neutrino Production Diagnostics with the Glashow Resonance

Abstract

We study the Glashow resonance ${\bar{\nu }}_e+e^{-}\to W^{-}\to$ hadrons at 6.3 PeV as diagnostic of the production processes of ultra-high energy neutrinos. The focus lies on describing the physics of neutrino production from pion decay as accurate as possible by including the kinematics of weak decays and Monte Carlo simulations of pp and p$\gamma$ interactions. We discuss optically thick (to photohadronic interactions) sources, sources of cosmic ray nuclei and muon damped sources. Even in the proposed upgrade IceCube-Gen2, a discrimination of scenarios such as pp versus p$\gamma$ is extremely challenging under realistic assumptions. Nonetheless, the Glashow resonance can serve as a smoking gun signature of neutrino production from photohadronic (A$\gamma$) interactions of heavier nuclei, as the expected Glashow event rate exceeds that of pp interactions. We finally quantify the exposures for which the non-observation of Glashow events exerts pressure on certain scenarios.

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Cited by in corpus (10)

• Detection of a particle shower at the Glashow resonance with IceCube
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• Unified thermal model for photohadronic neutrino production in astrophysical sources
• The flavor composition of ultra-high-energy cosmic neutrinos: measurement forecasts for in-ice radio-based EeV neutrino telescopes
• Two-detector flavor sensitivity to ultra-high-energy cosmic neutrinos
• Inferring astrophysical neutrino sources from the Glashow resonance
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• Neutrino Astronomy at High Energies - An Experimental Review
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